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Best waterproof phone 2021
It's fair to assume that electronics and water aren't the best of friends, but in recent years the idea of a phone falling into a body of the wet stuff isn't necessarily a death sentence anymore.
Manufacturers have been exploring ways to make their products more resistant to dirt, shock, extreme temperatures and moisture for years – GoPro cameras were born out of such a need – and nowadays there are established methods that help guarantee such tech is more resilient.
Originally, you had to look the likes of LifeProof and other specialist phone case makers to gain the necessary protection against the elements for your mobile; adding bulk to their otherwise sleek, lightweight designs and complicating access to ports and controls in the process.
More recently phones – particularly those in the flagship space – have benefitted from internal design changes and additions that help make them hardier, without impacting on their overall dimensions or aesthetics.
Motorola and Sony have led the charge in the mobile space when it comes to water-resistant phones. The use of both seals and hydrophobic coatings are essential to keeping your tech water and dust-free, and nowadays everyone from the likes of Apple and Samsung to OnePlus offer up at least one device with certified levels of ingress protection (also known as IP ratings).
Related: What is an IP rating? Waterproofing and water resistance explained
Based on the capabilities of the phone in question and the degree to which they are able to withstand contact with water (and dust), we've assembled a list of the best water-resistant phones you can get your hands on right now.
As mentioned, most reside within the flagship space but competent ingress protection has made its way into the mid-range market too, so keep your eyes peeled for more affordable devices that also cite an IP rating if you can't find what you're looking for here.
Best waterproof phones 2021
1. iPhone 12 (+ 12 Mini, 12 Pro & 12 Pro Max) – Best overall
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You might notice that Apple holds the tops spots on this list, but we promise this isn't a case of brand favouritism. While the Android phones further down all adhere to IP68 certification, Apple has gone above and beyond with the iPhone 12 (and 11) range.
Our pick of the bunch is the standard iPhone 12 but the iPhone 12 Mini, iPhone 12 Pro and iPhone 12 Pro Max all feature the same industry-leading water resistance; rated against up to 6 metres (approximately 19.7 feet) of fresh water for up to 30 minutes.
The standard iPhone 12 is our preferred pick of the range as it's not only a nice jump up from the iPhone 11 but also doesn't lose out on all that much compared to the pricier iPhone 12 Pro.
Highlights include its new iPhone 5-inspired design, its Super Retina XDR OLED display, Apple's A14 Bionic chip and Dolby Vision HDR video recording.
Read our full Apple iPhone 12 review
2. iPhone 11 Pro (& 11 Pro Max) – Superb all-rounder
While not quite as submersible as its 2020 successors, the iPhone 11 Pro line lands the number-two spot on our list, thanks to resistance in up to 13 feet for fresh water for up to 30 minutes.
As for the rest of the 11 Pro, while we're not fully on board with the 'Pro' naming, there's no doubt that at launch, this was the best iPhone you could opt for, and is still an excellent buy today.
We like the matte finish, which provides more grip than standard glass and helps negate fingerprints. The OLED screen is stunning, especially with iOS 13's Dark Mode, the cameras are excellent, performance is slick and battery life is better than any previous iPhone generation – there's a lot to like.
Still, it's a lot more expensive than the regular iPhone 11 which has the things that most people want and doesn't really break any new ground. It's not even 5G capable (again, look to the newer iPhone 12 line if that's the sort of functionality you're looking for).
Read our full Apple iPhone 11 Pro review
3. iPhone 11 – Well-rounded
Unlike the iPhone 12 line, Apple tiered the level of water resistance on its 2019 iPhones, with the non-Pro iPhone 11 coming in as a little less hardy than the fancier models.
While not quite as well-adapted as its Pro-branded siblings, the base iPhone 11 still totes above-average water resistance that works at up to 6.5 feet/2 metres of freshwater for 30 minutes.
The iPhone 11 didn't need to rewrite the smartphone rule book to be a winner. It simply needed to build on the success of the XR and it did exactly that.
It features a nice design which comes in various colours. Face ID is improved over the XR and the telephoto lens has been swapped for a more useful wide-angle lens. The screen still isn't OLED (check out the iPhone 12 if that's what you're after) but offers a decent experience anyway and performance is still top-notch – even when playing very demanding games.
All of this for a cheaper price than the iPhone XR, when it first arrived. Apple did it again.
4. Samsung Galaxy S21 (+ S21+ & S21 Ultra) – Best for Android
As mentioned earlier, the rest of the devices in this lineup, including the S21 line, are listed as being able to withstand the exact standards of IP68-certification – submerged in up to five feet (1.5 metres) of fresh water for up to 30 minutes.
Samsung takes the same superb balancing act that it struck with last year's Galaxy S20 series and updates the hardware.
As a result, you get the best performance found in an Android phone currently, a fresh new design, better battery life, the latest Android 11 (dressed in Samsung's own One UI 3.1, at launch) and integrated 5G.
Best of all, all this comes in a more affordable package than its predecessor.
Read our full Samsung Galaxy S21 review
5. OnePlus 8 Pro – Stunning display
The OnePlus 8 Pro is arguably the company's first full flagship, finally incorporating long-requested features like wireless charging and an IP68-certified rating to make it a genuine contender with the likes of Samsung's finest of 2020.
Understandably, the price has gone up accordingly, but even the base model – no slouch at 8GB RAM and 128GB storage – still represents serious value by flagship standards, meaning you will save at least some money by opting for OnePlus over most other manufacturers.
The 8 Pro's camera is the company's best yet and while it still lags behind rivals, OnePlus's imaging engineers have clearly worked hard to narrow the gap considerably. Throw in 5G, a great design and the best Android skin around and the OnePlus 8 Pro is easy to recommend to anyone who can afford it.
Read our full OnePlus 8 Pro review
6. Oppo Find X2 Pro – Best stills camera
The Oppo Find X2 Pro is a phenomenal phone by any measure. The 6.7in 10-bit 120Hz QHD+ panel is one of the best displays in any phone right now and Oppo backs it up with the fastest wired charging around at 65W and a top-tier camera that boasts two 48Mp lenses and up to a 10x hybrid zoom.
You'll have to live without wireless charging and the choice between bland grey ceramic or garish green or orange vegan leather finishes might leave some struggling to find a design that suits their style.
For pure performance though, the Find X2 Pro is still a force to be reckoned with: with all of the above plus a Snapdragon 865 chip, 512GB storage and 12GB RAM – you just have to be willing to pay the price, as it doesn't come cheap.
Read our full Oppo Find X2 Pro review
7. Samsung Galaxy Note 20 Ultra – Best for productivity
A true powerhouse – the Note 20 Ultra doesn't take any prisoners, with its flagship performance, greatly-improved camera (compared to the Galaxy S20 Ultra), low-latency S Pen experience and the sheer number of features it offers.
Samsung's One UI user experience is jam-packed with functionality without feeling overwhelming. You have control over pretty much every aspect of the phone and it's designed to help you get things done.
The pairing of S Pen and the updated Samsung Notes experience is a particular highlight, as is the tighter Microsoft integration. There's also the matter of DeX desktop experience – which is now fully-wireless with compatible displays.
Read our full Samsung Galaxy Note 20 Ultra review
8. Google Pixel 5 – Most compact
Google's first 5G flagship walks a different path to its predecessors, showcasing Android 11 to the best of its abilities but also shedding the more experimental features of previous generations and opting for more conservative hardware at the same time.
Its clean design and user experience are supported by a set of superb – and now more feature-rich – cameras, as well as an incredibly compact design and battery life that's actually usable.
Don't be put off by the literature on Google's website, the Pixel 5 is also confirmed to be IP68-certified (not just IPX8).
Read our full Google Pixel 5 review
9. Samsung Galaxy S20 – Great for ease of use
The best entry in the S20 series and simply Samsung's best phone of 2020. It's compact, powerful and packs a versatile camera system that may not match the top-tier S20 Ultra on zoom or detail but still meets – and sometimes beats – it across the rest of the board.
While battery life remains a slight concern, that's really the only major fault here. The Android ecosystem offers more for less elsewhere, but usually, without Samsung's level of prestige or polish, and in this case, we think that's worth paying for.
10. Sony Xperia 1 II – Great for multimedia
Sony's latest flagship doubles down on the unique attributes of 2019's Xperia 1, with an enhanced 21:9 4K HDR OLED display, a wealth of audio technologies (including a 3.5mm headphone jack) and a Sony Alpha-influenced triple-camera module.
It's augmented but clean take on Android includes meaningful improvements and despite not looking as competitive on paper as other Android flagships, its performance and battery longevity proved more than capable in testing.
Read our full Sony Xperia 1 II review
Related stories for further reading
Best iPhone 12 and 12 Pro cases in 2021
OnePlus announces Hasselblad partnership: OnePlus 9 arriving on March 23
Technical Guruji: What makes the Android more popular than iOS?
Pete Lau says no DxOMark review for the OnePlus 9 series; launch set for Mar. 24 in China


Given the shambles in Government since Jacinda Ardern returned from maternity leave, a show of unity by Winston Peters and James Shaw at the Prime Minister's major speech today was in order.
The political theatre is of greater value than the substance of the Prime Minister's speech, billed as "Our Plan".
And the timing of the speech, which was planned when the PM was on maternity leave, was fortuitous.
It may help to give a sense of coherence to the Government which has been looking fairly chaotic recently, particularly between Peters' New Zealand First and Labour.
Peters provided the preamble to Ardern's speech.
In it, he uttered the words we have not heard from him in a long time – "Labour." He did not refer to the Labour-led Government, a term which he now finds offensive given it subjugates the role of New Zealand First.
But he did refer to the Labour-New Zealand First Coalition. He said the Coalition was "unified".
Not quite unified enough for Peters to share the stage with the Greens after Ardern's speech, to take questions from the audience.
Ardern delivered her speech in Ted-talk-style, like the gifted communicator she can be.
And while it was important in terms of setting out priorities, nothing in it was new.
Under three themes, and 12 priority areas, it draws together various known promises from the disparate documents Ardern has long talked about as comprising the Government's programme: the two coalition and confidence and supply agreements, the Speech from the Throne, and the 100 days programme.
Ardern herself has developed the work plan and has given Cabinet committees responsibility to identify which policies come within their ambit and how progress on them can be measured every six months.
She revealed the plan with the enthusiasm of someone who believes she has done something remarkably new – which of course she hasn't.
Her work plan will necessarily be different to any other Government's because like every Government it is unique in its makeup, and has its own goals.
But the notion that this is the first time a Government has set objectives and will measure them every six months is nonsense, as is the claim that this is first Government of compassion.
She might think she is inventing the wheel but as anyone who followed Bill English's monitoring work in the Better Public Service programme and social investment knows, it has been invented before.
In fact her plan appears to be a hybrid of the thematic approach to policy honed by former prime minister Helen Clark and the very specific measures demanded by English's social investment and Better Public Service Targets approach.
Most of the problems of the Government in recent weeks have arisen from Coalition management, not because there was no plan.
Ardern's outline of the plan is to be welcomed. But it wont be a substitute for better management by the parties of Government.


The Find and Replace feature of Microsoft Excel is often needed in spreadsheets that contain a lot of data and workbooks. This feature scans your worksheet or workbook for specific words or phrases and provides that information in a list format. The "Replace" feature will change each instance of your "Find" phrase to a different set of text that you designate. "Ctrl" and "F" is the shortcut key to open the Find and Replace dialog box.
Open your Microsoft Excel file.
Press "Ctrl" and "F" to open the "Find and Replace" dialog box.
Enter text into the "Find what:" field. Click the "Options" button to add search criteria. Your options include searching one sheet or the entire workbook, searching by row or column or designating where to look.
Click the "Find Next" button to go through each instance individually.
Click the "Find All" button to generate a chart. This chart provides a listing of the row and column of each instance of the word you searched.
Click the "Replace" tab to change your text. Enter the text you want to find. Enter the text you want to replace it with. Click "Replace" to go through individually. Select "Replace All" to automatically change each instance.


Kitchen : Cupboard Covers Facelift Your Cabinets Prices Modern Cabinet Refacing Price To Reface Captivating Re Veneering Cost Refurbish Renovate Doors ~ Kioscopedia Inc.
Published at Thursday, February 07th, 2019 - 10:48:47 AM. Kitchen. By Albertina Carre.


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EspyRock
The best for music recommendations and rock news!
Tag Archives: Velvet Revolver
Album Review: Slash – Apocalyptic Love
If anyone's keeping score on who the most credible and respected former Guns N' Roses member is, it surely has to be Slash? While Axl descends further and further into madness with his appetite for destruction, Slash continues to make it look so easy. His self-titled debut album saw the top-hatted virtuoso call up some […]
Slash performs new song and covers Velvet Revolver on Guitar Center Sessions
Slash, alongside his band which features Alter Bridge vocalist Myles Kennedy and The Conspirators – Brent Fitz (drums) and Todd Kerns (bass), recently performed a Guitar Center session on DIRECTV where they performed their new song 'Not For Me' and a cover of Velvet Revolver's 'Fall To Pieces.' Watch the videos below and also stream […]
Scott Weiland announces his return to Velvet Revolver, Slash has no idea what he is talking about
Scott Weiland has revealed to ABC News Radio that he has reunited with Velvet Revolver but according to Slash, Velvet Revolver will not be going backwards and Scott Weiland is not part of their line-up. "We've all grown a lot," explains Weiland. "We're able to put egos and differences and old…conflicts aside and so that's […]
Velvet Revolver to release Live In Germany DVD, performance streaming online
Velvet Revolver have announced that they will release a new DVD titled 'Let It Roll – Live In Germany' on the 25th May. The DVD was recorded in Cologne, Germany on the 29th March 2008, days before Scott Weiland departed the band. The full track listing and artwork can be viewed below. The concert was […]
Corey Taylor and Duff McKagan may form new supergroup with material already written
Corey Taylor went on the record on Friday by stating that he will not be part of Velvet Revolver as the rumour mill continues to spin that he will still be joining even after all parties involved had already killed the possibility. Mark Hoppus of Blink-182 questioned the vocalist on his show, Hoppus On Music, […]
Velvet Revolver have full album recorded with Corey Taylor
In a recent Lokaos.com.br interview with Velvet Revolver drummer Matt Sorum, Sorum reveals that bringing in Corey Taylor was his idea. He goes on to state that Slash was the only one who didn't like the material but they "could put the album out tomorrow. It's done." If Slash changes his mind then we could […]
Myles Kennedy will not be joining Velvet Revolver
For some time we have been waiting on the word of who will join Velvet Revolver and front the band after Scott Weiland left the band. After the announcement that Myles Kennedy would front Slash's solo band on tour, many fans hoped this would lead to Myles joining Velvet Revolver. Some may already know that […]

redpajama_set_name: RedPajamaCommonCrawl


Owners Jon and Jan Brieger welcome you to the Redbud Cafe!
Potters by trade, Jon and Jan have been crafting pottery by hand and selling their work at Brieger Pottery in Blanco, Texas, for over 15 years. Both the pottery shop and the cafe are located in the building that originally housed the town's hardware store. The cafe now opens onto the pottery shop – right next door.
Watch this site for updates on menu specials, our music calendar, and special events at Redbud Cafe.
I have always felt that clay and dough belong together.
YES! they do… and they are right next door to one another!
I visited your resturant last week and loved it. I have it featured today on my personal blog and the blog I write for the San Antonio Express News. Hope the publicity will bring in some business…you have a great place!
Thanks for the positive feedback and spreading the word. Hope to see you again soon!
I've been to your place a few times and have enjoyed it every time. The relaxed atmosphere and the menu variety and quality are really enjoyable. The only complaint I've ever had is the crowds, which is a testament to the good food. I'll be bringing friends with me this weekend. Thanks for what you do!


On May 9, 2013, the Commission held its regularly-scheduled agenda meeting. No telecommunications items were discussed on the regular agenda, but the CPUC was authorized on the consent agenda to file comments on the FCC's proposed rulemaking to consider 9-1-1 reliability issues. The Commission continued its hold on several important items, including the draft Order Instituting Rulemaking ("OIR") to implement franchise renewal provisions of the Digital Infrastructure and Video Competition Act of 2006 ("DIVCA") and the Proposed Decision modifying requirements for CPCN and WIR holders or applicants. These and other items of interest are discussed in further detail below.
CPUC to File Comments with FCC Addressing 9-1-1 Reliability (Item 35, approved on consent agenda) – This item authorizes the CPUC to file comments in response to the FCC's Notice of Proposed Rulemaking in the Matter of Improving 9-1-1 Reliability. The FCC's Notice requested comments on approaches to ensure that infrastructure is in place to provide for continued availability of the nation's 9-1-1 system, especially during times of major disaster. The CPUC's comments will: (1) provide support for the FCC's technology-neutral definition of "9-1-1 service provider"; (2) urge the FCC to adopt technology-neutral minimum back-up power requirements for 9-1-1 networks; (3) provide for the adoption of a federal certification requirement where providers certify to the reliability of their 9-1-1 systems; and (4) present a proposal that the FCC should provide states with timely access to carrier reports pertaining to 9-1-1 networks in their state.
Rulemaking to Modify Video Franchise Renewal Procedures (Item 5, held by Staff until 5/9/13) – This item would adopt a new rulemaking to evaluate the terms under which state video franchisees can seek renewal of their authority under DIVCA. The Draft OIR outlines an approach to renewal that harmonizes Public Utilities Code Section 5850(b) with the requirements of federal law. As with the application process under DIVCA, the OIR envisions a relatively informal, largely ministerial process. The proposal would permit comment on franchise renewals, but comments would be limited to whether or not an application is complete – the Commission would not be exercising discretionary authority over franchise renewals with reference to policy considerations.
Revisions to the Certification Processes for Telephone Corporations Seeking or Holding CPCNs and WIRs (Item 33, held by Staff until 5/9/13) – This item would adopt revisions to the certification process for telephone corporations seeking or holding Certificates of Public Convenience and Necessity ("CPCN") and wireless carriers seeking or holding Wireless Identification Registration ("WIR"). The changes to the certification processes are intended to increase accountability for carriers, reduce the need for enforcement actions to be brought, and improve the Commission's ability to collect fines, penalties, and bring restitution. The Proposed Decision would establish a Phase II of the proceeding to determine performance bond requirements, as discussed below.
Sprint's Application for Indirect Transfer of Control (Item 4, held by Sandoval until 5/23/13) –This Proposed Decision would authorize a transaction that allows Starburst II, Inc. ("Starburst II") to become the direct parent of Sprint Nextel Corporation ("Sprint Nextel") and the indirect parent of Sprint Nextel's wholly-owned subsidiary, Sprint Communications Company, L.P. ("Sprint Communications"). Starburst II is a newly formed entity of SoftBank Corp. ("SoftBank"). Through Starburst II, SoftBank will invest $20.1 billion in Sprint Nextel and indirectly acquire approximately 70% of the shares of Sprint Nextel. SoftBank is a publicly-traded holding company organized under the laws of Japan and headquartered in Tokyo. SoftBank's various subsidiaries and affiliates are engaged in a range of information technology and Internet-related businesses in Japan. SoftBank's wholly-owned subsidiary, SOFTBANK MOBILE Corp. is currently Japan's third largest wireless carrier. SoftBank holds no authorizations from the Commission, but one of its subsidiaries holds an FCC authorization to provide a private line service to another wholly-owned subsidiary of SoftBank.
Sprint Communication's application was protested by the National Asian American Coalition, Latino Business Chamber of Greater, L.A., and Ecumenical Center for Black Church Studies (collectively,"NAAC"). The application was also protested by The Center for Accessible Technology, Division of Ratepayer Advocates, The Greenlining Institute, The National Consumer Law Center, and The Utility Reform Network (collectively, the "Consumer Groups").
NAAC's protested on the basis that the applicants had not adequately addressed the public interest benefits related to the proposed acquisition. NAAC also detailed additional issues for the Commission to examine, including Sprint's plans for accelerating broadband deployment, specific devices and services that Sprint planned on offering as a result of the acquisition, the CPUC's jurisdiction over the wireless component of the acquisition, and the planned public benefit to California's poverty-stricken ratepayers. The Consumer Groups raised concerns about the potential impacts that the proposed transaction would have on ratepayers. Specifically, the Consumer Groups were concerned with the impact on competition, quality of service, state and local economies, and the Commission's ability to regulate public utilities. The Consumer Groups urged the Commission to further investigate to ensure that risks to Sprint's customers are mitigated.
The Proposed Decision would find that the protests fail to point to any specific instance where the applicants failed to meets its public interest obligation. In addition, the Proposed Decision notes that the protests do not identify general or specific harms that would impact ratepayers in California. Instead, the Proposed Decision would conclude that there is no aspect of the transaction that would be adverse to the public interest and that a change in ultimate ownership would not negatively impact Sprint Communication's operations or financial status. Moreover, the Proposed Decision would find that the applicants have demonstrated that the acquiring company, Starburst II, has sufficient managerial and technical expertise, as well as sufficient financial resources to operate the acquired carrier. In addition, the Proposed Decision determines that the transfer of control would be appropriate and consistent with the Commission's technical, safety, and environment requirements for granting CPCN authority to a telecommunications carrier.
Verizon's Deviation from Public Utilities Code Section 320 (Item 14, held by staff until 5/23/13) –This Draft Resolution would approve Verizon California Incorporated's ("Verizon") deviation from Public Utilities Code Section 320 for overhead distribution facilities installed without Commission approval in 2004. Section 320 requires, where feasible, the undergrounding of all electric and communication distribution facilities to be erected in proximity to any highway designated as a state scenic highway. Utilities may request authority for deviation through an advice letter process.
The Draft Resolution would determine that approving the deviation is appropriate because the cost of underground installations would have been twelve times the cost of an aerial installation. It explains that the CD Staff conducted a site inspection of the overhead distribution facilities and identified problematic areas that could be resolved to address safety and aesthetic concerns. In addition, the Draft Resolution would also impose penalties on Verizon for non-compliance with Commission rules. Therefore, the Draft Resolution would grant Verizon's request for waiver of Section 320 after documented completion of the following conditions: (1) replacement of all aluminum cable dampers that are less prone to glare; (2) the completion of an audit for compliance with G.O. 95; (3) the development of a plan for future construction of overhead distribution facilities within California; and (4) payment of a $5,000 penalty for failure to comply with Section 320. These conditions must be met within one year after this Draft Resolution is approved.
Proposed Legislation on 911 Service, AB 911 (Bloom) (Item 40, held by Staff until 5/23/13) – This bill would establish 911 emergency call technology requirements for multiline telephone systems ("MLTS"). These requirements would become effective on January 1, 2019. Specifically, this bill would require an MLTS operator in an area that has enhanced 911 capability to ensure that emergency calls placed from any telephone station on the MLTS is routed to a public safety answering point ("PSAP") that provides automatic location information or automation number identification to the 911 network that connects to a PSAP. This bill would also authorize civil penalties against MLTS providers who do not comply with the requirements outlined in the bill.
Proposed Legislation on the California Advanced Services Fund, AB 1299 (Bradford) (Item 45, held by Staff until 5/23/13) – This bill would require the Commission to develop, implement, and administer the California Advanced Services Fund to encourage deployment and adoption of broadband to Californians living in publicly supported housing communities in urban regions without increasing, or assessing a new surcharge. The bill is related to concerns raised by various Legislators that certain areas of Los Angeles are inadequately served with broadband.
Proposed Legislation on Service Interruptions, SB 380(Padilla) (Item 47, held by Staff until 5/23/13) – This bill requires a governmental entity to obtain an order, signed by a judicial officer, before it can interrupt communications services for the purpose of public safety or to prevent the use of communications service for an illegal purpose. Interruption of communications services must be limited to as long as reasonably necessary or once the danger justifying the interruption has abated.
Proposed Legislation on Intervenor Fees, AB 995 (Frazier) (Item 42, withdrawn) – This bill would require the Commission to adopt rules establishing standards to verify that a customer representative is authorized by consumers, customers, or subscribers of any of the utilities. In addition the bill would revise the definition of "substantial contribution" to require a Commission finding that the customer's participation promoted a public purpose that directly benefits other customers. The bill would also prohibit the total amount of the Commission annually awards for intervenor compensation from exceeding the mean average of awards for the previous 3 calendar years.
Proposed Legislation on Earthquake Early Warning System, SB 135 (Padilla) (Item 46, held by staff until 5/23/13) – This bill would require the Office of Emergency Services to coordinate with specified state and federal entities to establish an early earthquake warning system in California. This bill relies on the expansion of the current California Integrated Seismic Network and will require the development of technology to improve the detection of earthquakes.
The Safety and Enforcement Division ("SED") provided an update on the limousine tragedy that occurred on May 4, 2013. The SED explained the Commission's role in regulating limousines, which is to inspect licensing, insurance, and certification issues.
Commissioner Sandoval expressed concern regarding the Commission's lack of oversight over stretch limousines. She noted that most limousines are regular town cars that have been "stretched" through the addition of steel and other material. She was particularly concerned with the safety implications of "stretching" these vehicles and the lack of oversight over companies who provide these expansions, which may or may not comply with a manufacturer's motor and electrical plans.
The SED also provided a presentation on vegetation management to provide safe clearance for transmission lines. The presentation highlighted the relevant state and federal regulations governing clearance requirements that help to prevent fire hazards and outages caused by vegetation.
Commissioner Peterman attended a forum at the University of Southern California regarding the role of the government in facilitating innovation in communications and in establishing consumer protection. She also noted several telecommunication-related events taking place in the next few weeks, including eight Public Participation Hearings to discuss revisions to the LifeLine program and workshops to discuss the development of a Speech Generating Device program for the deaf and disabled.


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What is Theosophy?
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Krotona Library
Krotona Library was founded in 1912 when Krotona was located in Hollywood, and was moved to Ojai along with the Institute in 1924. The library emphasizes the ageless wisdom tradition, or Theosophy, and spiritual traditions of East and West. Students and research scholars are welcome.
Explore the ageless wisdom tradition, Theosophy, and spiritual traditions of East and West.
Our collection includes nearly 8,000 book titles and contains a wide range of materials including texts, journals, and study guides on Our collection includes nearly 8,000 book titles and contains a wide range of materials including texts, journals, and study guides on
meditation and healing
science and spirituality
Browse our titles in the Online Catalog.
The Joy Mills Collection
The Krotona Library hosts an extensive collection of lectures, essays, articles, photographs, correspondence, and over 500 annotated books by distinguished Theosophical scholar Joy Mills.
The collection is available to scholars, writers, researches and students.
"Our immediate task is to effect within ourselves such a transformation as will bring about the birth of a new individual." —Joy Mills
Krotona library is open to all. Visitors may explore the collection, relax in the peaceful atmosphere of the library, study in comfortable surroundings, and check out interesting books.
The Library loans its collection to residents of Ventura and Santa Barbara counties, in addition to serving Krotona's resident scholars, faculty and students.
Membership Fee: $20 per year
H. S. Olcott Memorial Library (Wheaton, IL)
An expanded theosophical resource is available through the collection of the Henry S. Olcott Memorial Library in Wheaton, Illinois. For more information visit the web site of the Olcott Library. You may also be interested in the The Adyar Library and Research Center at the Theosophical Society International headquarters in Chennai, India.
Borrowing Policy
Books: 1-3 titles for up to 4 weeks.
Book renewal is an additional 4 weeks if the book is not on hold and may be requested by phone or email.
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\section{Introduction}

Since the members of an open cluster are assumed to be of same age and chemical
composition, these stars are currently used to test the validity of  stellar evolution
theories\footnote{Some of the most recent detailed works on such critical tests
of stellar evolution in open clusters are due to  Nordstr\"{o}m {\al} (1997) and
Pols {\al} (1998).}, mainly because main sequence stars define a tight sequence
in a colour-magnitude diagram (CMD). Unfortunately, this tightness is sometimes
misleading  because of the contamination by field stars, the presence of unresolved binaries
and also the influence of stellar rotation on the location of massive stars in CMDs. \\
Alternatively, well-detached binaries are powerful tests when fundamental
parameters are accurately known (see the comprehensive review by Andersen 1991
on double-lined eclipsing binaries). Unfortunately, the determination of
the chemical composition often remains a difficult and unresolved issue.
It appears therefore that  a better test could be performed by combining both
advantages, that is, testing the tracks with well-detached double-lined binaries
which are members of open clusters. \\
The work developed in this paper is the application of this idea to three
well-detached binaries members of the Hyades: 51 Tau, V818 Tau,
and $\theta^2$ Tau.
Torres {\al}, 1997 ([TSL97a], [TSL97b] and [TSL97c]) obtained the
first complete visual-spectroscopic solutions for these systems, from which they
carefully derived very accurate parallaxes and individual masses. They also
gathered some individual photometric data in the Johnson system.
Furthermore, we found useful trigonometric parallaxes information in the
Hipparcos catalogue (ESA, 1997). By combining the two sources of data,
we investigate the influence of the Hipparcos parallaxes on our method which was
developed to test stellar evolutionary models in HR diagrams.  \\
According to Leitherer {\al} (1996), the most widely used stellar
theoretical tracks in the literature are those computed by the Geneva group
(Schaller {\al} 1992, Schaerer {\al} 1993a, 1993b, and Charbonnel
{\al} 1993) and the Padova group (Bressan {\al} 1993, Fagotto {\al} 1994a,b
\footnote{High metallicity tracks (Z $=$ 0.10) are also available for the Padova
group (Fagotto {\al} 1994c), and the Geneva group (Mowlavi {\al} 1998),
but they are not relevant for the expected Hyades metallicity.}).
We also used the stellar tracks from Claret \& Gim\'enez (1992) (CG92
thereafter). The tests presented in the next section are
done with these 3 series of stellar tracks to assess the possible
systematics introduced by the  use of a single set.\\
The test we want to perform has two aims. Firstly it has to check whether the two
components of the systems are on the same isochrone, i.e. on a line defined
by the same age and the same chemical composition for the two single stars.
Secondly, as all the selected stars are members of the Hyades  whose \met has been
well measured, we can also check that the predicted \met from theoretical models
are correct. Therefore, if one of these two criteria is not clearly fullfilled by
a given set of tracks, then these models have obvious problems since they do not
account for several observational constraints (namely the \met and/or the photometric
data).\\
We would like to emphasize that we do not claim that the
6 selected Hyades stars allow us to test without ambiguity any set of theoretical
stellar tracks. Since the data are presented in colour-magnitude diagrams,
we are in fact testing not only the validity of the tracks (computed in terms of
effective temperature and bolometric luminosity in the HR diagram) but also
the validity of
the photometric calibrations, and disentangling the relative influence of both is
a tricky task.
However, since we use the Basel Stellar Library (BaSeL) photometric calibrations,
extensively tested and regularly updated for a larger set of parameters (see Lejeune
{\al} 1997, Lejeune {\al} 1998, Lastennet {\al} 1999 and Lejeune {\al} 1999), we
assume that the calibrations are reliable for our purposes.
Moreover, it is worth noticing that in the range of interest  of the  (B$-$V) colour
in the present work ([0.15, 1.25] mag.), the agreement between the various extant
calibrations, i.e., the transformations between theoretical $T_{\rm eff}$ and
observational (B$-$V) colour, is quite
good around  metallicities close to solar (see, for example, Alonso {\al} 1996 and Fig. 8
of Flower 1996 for some comparisons). Significant differences do occur at cooler
temperatures, but they are not relevant for the present study.
For these reasons, we will assume that the calibrations from the BaSeL
models are reliable enough for this work.\\
Another crucial point is the question of reddening. The Hyades open cluster does not
show any evidence for reddening (E(B$-$V)$=$0.003$\pm$0.002, Taylor 1980), consequently
E(B$-$V) is assumed to be consistent with  0 in this paper. \\
The paper is organised as follows: Sect. 2 is a brief description of the method
used to produce confidence level contours, Sect. 3 is devoted to the study of each
binary, completed by comments on the influence of the Hipparcos parallaxes on
the location of the 6 stars in a mass-luminosity diagram. Finally, Sect. 4 draws our
general conclusions.

\input{table1.tex}

\section{Statistical method description}

It is not an easy task to disentangle  \met and  age effects in a colour-magnitude
diagram  with only two stars, particularly if they both lie close to the
main sequence. This difficulty is due to the degeneracy between these two
quantities in this area of the CMD.
For this reason, any analysis of binary star data should be presented in the
(metallicity, age) plane.
In order to derive simultaneously the \met (Z) and the age (t) of the system,
we minimize the $\chi^2$-functional defined as:

\beqa
\chi^2 (t, Z)  & = &  \sum_{i=A}^{B} \left[ \left(\frac{\rm M_V(i)_{\rm mod} -  M_V(i)}
{\sigma(\rm M_V(i))}\right)^2 \right.  \nonumber \\
 &  &+ \left.  \left(\frac{\rm (B-V)(i)_{\rm mod} - (B-V)(i)}{\sigma(\rm (B-V)(i))}\right)^2 \right]
\eeqa
where $A$ is the primary and $B$ the secondary component. M$_V$ and (B$-$V) are the observed
values (more details will be given later on M$_V$), and M$_V$$_{\rm mod}$ and
(B$-$V)$_{\rm mod}$ are obtained from the synthetic computations of the BaSeL models
using a given set of stellar tracks.

A similar method has already been developed and used by Lastennet {\al} (1996)
and by Lastennet \& Valls-Gabaud (1999) for
HR diagrams. Equation 1 simply means that the best $\chi^2$ is obtained when an
isochrone is close to both stars A and B in the CMD.
With $n=4$ observational data (M$_{\rm V}$ and B$-$V for each star) and  $p=2$ free
parameters (age t and metallicity Z), we expect to find a $\chi^2$-distribution with
$q=n-p=2$ degrees of freedom. Finding  the central minimum value $\chi^{2}_{\rm min}$,
we form  the $\chi^2$-grid in the (metallicity, age)-plane and compute the boundaries
corresponding to 1$\sigma$, 2$\sigma$, and 3$\sigma$ confidence levels.
We do not use any additional information in the $\chi^2$ functional such as radii
or masses since (1) these are not always available at the same time, and (2) they
should be predicted by the tracks (Lastennet \& Valls-Gabaud 1999).

\section{Tests with well-detached binaries}

In this section tests of the widely used theoretical stellar tracks are presented. They
are based on a few number of binary systems belonging to the Hyades open cluster, for
which Johnson BV photometric magnitudes and accurate mass estimates are available: 51
Tau, V818 Tau, and $\theta^2$ Tau. V818 Tau is the only eclipsing binary among these
three systems.
Contrary to Lastennet \& Valls-Gabaud (1999) where tests are presented in the
theoretical HR diagram, our tests are performed in the CMD. \\
The main advantage to study such binaries, members of an open cluster,
is that the heavy element abundance of the Hyades has been extensively studied and
estimated by different authors. As a matter of fact, the \met of the binaries studied
in Lastennet \& Valls-Gabaud (1999), mainly from the field, was seldom known.
The more recent determinations of the Hyades \met have been reviewed by Perryman
{\al} (1998): [Fe/H] $=$ 0.14 $\pm$ 0.05, i.e. Z $=$ $0.024^{+0.0025}_{-0.003}$ assuming
a subsolar helium abundance (Y $=$ 0.26), which is the value found by Lebreton {\al} (1997)
in order to reproduce the Hyades main sequence, with an uncertainty of about 0.02 resulting
both from the error bars of the Hyades members in the HR diagrams and from the observational
uncertainty on [Fe/H].
A second advantage is that very accurate parallaxes are now available from Hipparcos
for these three systems (the last estimation of the Hyades distance from Perryman {\al}
(1998) is: d $=$ 46.34 $\pm$ 0.27 pc). Moreover, we pay attention to the quality of the
Hipparcos results using the indicators F1 (percentage of rejected observations
\footnote{This field gives the percentage of data that had to be rejected in order
to obtain an acceptable astrometric solution.}) and F2 (goodness-of-fit statistic)
in order to ensure that the parallaxes are reliable. The data used in the present work
are gathered in Table 1.

Absolute magnitudes of each binary component are directly inferred from
Hipparcos parallaxes $\pi$ and visual magnitudes V:
\begin{equation}
M_V = V + 5 + 5 \times \log (\pi)
\end{equation}
\begin{equation}
\Delta M_V = \Delta V + \frac{5}{\ln(10)}
\times  \frac{\Delta(\pi)}{\pi}
\end{equation}

We do not take into account the Lutz--Kelker correction because relative
errors on parallaxes, $\sigma_{\pi}$/$\pi$, are always smaller than 10 \%:
respectively 4.5 \%, 5.8 \% and 3.8 \% for 51 Tau, V818 Tau and $\theta^2$ Tau.
Therefore the correction can be neglected as noted by Brown {\al} (1997).
In Table 1, the systematically larger distance found by Torres {\al} is, at
least in part, caused by the fact that the PPM proper motions that they used
(see Schwan 1991 and references therein) are almost all smaller than those of
Hipparcos (see Perryman {\al} 1998 for details).

\subsection{Results for 51 Tau}

The 51 Tau system is a spectroscopic binary and also a visual binary resolved by
speckle interferometry.
\begin{figure*}[htb]
\centerline{\psfig{figure=51Tau.ps,height=11.truecm,rheight=11.5truecm,angle=-90.}}
\caption{51 Tau system: influence of the Hipparcos parallax on the contour
levels derived from the Geneva tracks. The photometric locations of each single
star in the CMD are from Torres {\al} [TSL97a], except the absolute magnitudes
$M_V$ in the {\it bottom panel} which are derived from the Hipparcos parallax.
The correspondence between isochrones and symbols are directly given on the
plots. For instance, the best fit isochrone ({\it solid line} in the CMD) is defined by
Z $=$ 0.020, log t $=$ 8.88. In isocontours plots, the parameter values corresponding to
the best fits ($\chi^2_{\rm minimum}$) are marked by {\it open circles}. The metallicity--age pair
(Z $=$ 0.024, log t $=$ 8.80) from Perryman {\al} (1998) for the Hyades is shown for
comparison ({\it star} symbol). It is important to notice that all the isochrones inside the 1$\sigma$
confidence levels are also good fits: an older isochrone is also a possible fit
(e.g. the isochrone corresponding to the {\it triangle} defined by Z $=$ 0.015 and log t $=$ 9).
A comparison between {\it upper and bottom panels} shows that the 1, 2, and 3$\sigma$ contour
levels (respectively {\it solid}, {\it dashed} and {\it dot-dashed lines}) are not significantly
modified. Vertical lines in contour levels diagrams show the observational limits for the
\met of the Hyades.}
\label{f:51Tau}
\end{figure*}
\begin{figure*}[htb]
\centerline{\psfig{figure=51Tau_PC.ps,height=11.truecm,rheight=11.5truecm,angle=-90.}}
\caption{51 Tau system: Padova ({\it upper panels}) and CG92 tracks ({\it lower panels})
both taking into account the Hipparcos parallaxes.
The photometric locations of each star in the CMD are from Torres {\al} [TSL97a],
but the absolute magnitude $M_V$ is derived from the Hipparcos parallax.
As in Fig. 1, vertical lines in contour levels diagrams show the observational limits of
the \met of the Hyades, and the correspondence between isochrones and symbols are directly
given on the plots. The best fits ($\chi^2_{\rm minimum}$) are marked by {\it open
circles} (Padova: Z $=$ 0.017, log t $=$ 8.90, CG92: Z $=$ 0.018, log t $=$ 8.92), but good fits
can also be obtained with other isochrones: for example, the isochrones corresponding to the
{\it star} (log t $=$ 8.80 and Z $=$ 0.024, from Perryman {\al}, 1998) and to the {\it triangle}
(Padova: Z $=$ 0.017, log t $=$ 8.95, CG92: Z $=$ 0.015, log t $=$ 9.01), slightly older and more
metal poor than the best solution. In the CG92 diagrams ({\it lower panels}),
the {\it dotted line} isochrone (Z $=$ 0.017, log t $=$ 8.90) corresponds to the {\it diamond symbol}
which is very close to the best solution ({\it open circle}). However, the two isochrones are quite
different. In the CG92 CMD ({\it right bottom panel}), the small kink around B$-$V$=$0.4
is not due to the colour transformation but to the CG92 model at 1.41$M_{\odot}$.}
\label{f:51Tau_PC}
\end{figure*}

In order to address the question of the effect of the Hipparcos parallaxes on
our results, we first need
to present what  the results are without using these new parallaxes.
Figure \ref{f:51Tau} shows both the isocontours and CMD without using
Hipparcos ({\it upper panels}) and with Hipparcos parallaxes ({\it lower
panels}). The effect of using the Hipparcos parallaxes is hardly visible
on the results, in particular the shapes of the isocontours are not modified
a great deal.
Actually, the difference between the distance from Torres {\al} 1997
(d $=$ 55.8 $\pm$ 1.8 pc from the orbital parallax) and the distance derived from
Hipparcos (d $=$ $54.8^{+2.6}_{-2.4}$ pc) is rather small.
Since the errors on  distance are slightly larger with Hipparcos data, the
error bars estimates are slightly larger on the $M_V$ axis. \\
As mentioned previously, the more recent determinations of the Hyades \met have
been reviewed by Perryman {\al} (1998): [Fe/H] $=$ 0.14 $\pm$ 0.05 (i.e:
Z $=$$0.024^{+0.0025}_{-0.003}$). These constraints are shown in the (Z, age)-plane
as vertical lines. Torres {\al} (TSL97a) adopt [Fe/H]$_{\rm Hyades}$ $=$ 0.13 (following
 Cayrel {\al} 1985, Boesgaard 1989 and Boesgaard \& Friel 1990) and hence
 Z $=$ 0.027, which is about the upper limit quoted by  Perryman {\al} (1998).
From the $\chi^2$-contours in Fig. \ref{f:51Tau} and Fig. \ref{f:51Tau_PC}, one can
see that the stellar evolutionary tracks from Geneva, Padova and CG92 yield acceptable
and essentially equivalent fits of isochrones in agreement with the Hyades metallicity.
However, the preferred solution (i.e. with the minimum $\chi^2$-value) in the sets of
tracks points systematically to a smaller \met than expected
(cf. in each Z--age diagram the location of the {\it open circle}, best fit,
in comparison with the \met  constraints shown with vertical lines). \\
Since the masses of the two components of 51 Tau are known to a good accuracy
(respectively 7\% and 12\%), to check that the predicted masses are in
agreement with the measured masses is one more stringent test.
The best Geneva fit sligthly underestimates the masses of 51 Tau (by 0.5$\sigma$
for the primary and 1$\sigma$ for the secondary component) as well as the Padova best
fit (respectively 1$\sigma$ for the primary and $\sim$1.2$\sigma$ for the secondary)
and CG92 (respectively 0.5$\sigma$ for the primary and 1$\sigma$ for the secondary)
which means that these models are able to reproduce to a satisfying level the stellar
masses in the mass range of 51 Tau (see Table 2 for details).
The agreement is even better if we take into account
the following point. When spectroscopic and astrometric orbital elements are known,
one can derive the mass of each component, according to an hypothesis on the distance
(i.e. the parallax). Hence, if we keep all the orbital parameters (period, eccentricity,
velocity amplitude, ...) as given in [TSL97a] and take the Hipparcos parallax value of
51 Tau, one derives (from Eq. 2 in [TSL97c]) the new masses M$_A$$\simeq$1.66$M_{\odot}$
and M$_B$$\simeq$1.40$M_{\odot}$, values that are even better matched by the three sets
of theoretical models.
\begin{table}[htb]
\caption[]{Comparison of theoretical mass estimates from isochrone age fitting
of the system 51 Tau with the values of Torres {\al} [TSL97a].}
\begin{flushleft}
\begin{center}
\begin{tabular}{ccccc}
\hline\noalign{\smallskip}
 & [TSL97a]  & Geneva$^{a}$ & Padova$^{a}$ & CG92$^{a}$ \\
\noalign{\smallskip}
\hline \noalign{\smallskip}
\noalign{\smallskip}
A & 1.80$\pm$0.13 & 1.74$\pm$0.06 & 1.67$\pm$0.04 & 1.72$\pm$0.05 \\
B & 1.46$\pm$0.18 & 1.27$\pm$0.05 & 1.24$\pm$0.04 & 1.28$\pm$0.05 \\
\noalign{\smallskip}\hline
\end{tabular}
\end{center}
\smallskip
$^{a}$ 1$\sigma$ interval (this work). \\
\end{flushleft}
\end{table}
Assuming the most conservative \met values of the Hyades,  a close inspection of
the isocontours derived from the Geneva models reveals that the contours provide an age estimate
-- at the 1$\sigma$ level -- between log t $=$ 8.6 and 9.0 years (i.e. between 0.4 $\times$
$10^9$ and $10^9$ years).
A similar work with the Padova tracks give an age between log t $=$ 8.5 and 9.05,
and with CG92 between log t $=$ 8.75 and 9.05 years. As summarized in Table 3, these
values are in good agreement with the age estimation of Perryman {\al} (1998): log t
$=$ $8.80^{+0.02}_{-0.04}$, inferred from the isochrone fitting technique with the CESAM
stellar evolutionary code (Morel 1997).
\begin{table}[htb]
\caption[]{Comparison of theoretical age estimates from isochrone
age fitting of 51 Tau with Perryman et al's determination.}
\begin{flushleft}
\begin{center}
\begin{tabular}{ll}
\hline\noalign{\smallskip}
Stellar models & log(age) [yrs] \\
\noalign{\smallskip}
\hline\noalign{\smallskip}
\noalign{\smallskip}
Geneva$^{a}$ &  [8.60, 9.00] \\
Padova$^{a}$ &  [8.50, 9.05] \\
CG92$^{a}$   &  [8.75, 9.05] \\
CESAM$^{b}$  &  [8.76, 8.82] \\
\noalign{\smallskip}\hline
\end{tabular}
\end{center}
\smallskip
$^{a}$ 1$\sigma$ interval (this work), assuming
0.021$<$$Z_{\rm Hyades}$$<$0.026. \\
$^{b}$  Perryman {\al} (1998). \\
\end{flushleft}
\end{table}

\begin{figure*}[htb]
\centerline{\psfig{figure=V818TauP.ps,height=11.truecm,rheight=11.5truecm,angle=-90.}}
\caption{V818 Tau system: influence of the Hipparcos parallaxes on the contour
levels derived from the Padova tracks. The photometric locations of each star in the
CMD are from Torres {\al} [TSL97a], except the absolute magnitude $M_V$ in the
{\it bottom panel} which is derived from the Hipparcos parallax.
The best fit isochrones ({\it solid lines}) are defined by Z $=$ 0.033, log t $=$ 9.79
(with Torres {\al} parallaxes, {\it upper CMD}) and Z $=$ 0.033, log t $=$ 7.30 (Hipparcos,
{\it bottom CMD}). It is crucial to notice that all the isochrones inside the 1$\sigma$ confidence
levels are also good fits.
Vertical lines in contour levels diagrams show the observational limits for the \met of the Hyades.
The metallicity--age couple (Z $=$ 0.024, log t $=$ 8.80) from Perryman {\al} (1998) for
the Hyades is also shown for comparison ({\it triangle}). The corresponding isochrone
({\it dashed line}) clearly does not fit the system.
}
\label{f:V818Tau}
\end{figure*}
Finally, we would like to point out the need of new photometric data: the uncertainty
on the Johnson (B$-$V) colour of the faintest star is larger by a factor of 4 than
the primary. So, even if it appears clearly that the three sets of tracks do not fail
the test, accurate (B$-$V) data for the less massive component at the same level as
the primary should reduce the extent of the contours, allowing to perform more
stringent tests.

\subsection{Results for V818 Tau}

\begin{figure*}[htb]
\centerline{\psfig{figure=V818_mr.ps,height=11.truecm,rheight=10.5truecm,angle=-90.}}
\caption{V818 Tau system in a Mass-Radius diagram where all the isochrones are derived from
the Padova tracks.
The mass of each star is from Peterson \& Solensky (1988), as quoted by Torres {\al} [TSL97a],
and the radius is from Schiller \& Milone (1987).
In the {\it left panel}, the {\it solid line} isochrone (log t $\simeq$ 7.30, Z $\simeq$ 0.033)
is the best fit isochrone shown in the CMD of Fig. 3. Even if this isochrone allows to predict the
correct mass for each component, it clearly does not fit V818 Tau in the mass-radius diagram.
In the {\it right panel}, four different isochrones are shown for comparison: with a high
metallicity (Z $=$ 0.1) for two ages, t $=$ 0 ({\it solid line}) and t $=$ $10^9$ yrs ({\it dashed
line}) and with a very low metallicity (Z $=$ 0.0004) for the ages t $=$ 0 ({\it solid line}) and
t $=$ $10^9$ yrs ({\it dashed line}). There is no Padova isochrone which is able to fit
simultaneously both components of V818 Tau in the mass-radius diagram.
}
\label{f:V818_mr}
\end{figure*}
\begin{figure*}[htb]
\centerline{\psfig{figure=Theta02Tau.ps,height=11.truecm,rheight=11.5truecm,angle=-90.}}
\caption{$\theta^2$ Tau system: influence of the Hipparcos parallaxes on the contour
levels derived from the Geneva tracks. The photometric locations of each star in the
CMD are from Torres {\al} [TSL97a], except the absolute magnitude $M_V$ in the {\it
bottom panel} which is derived from the Hipparcos parallax. Vertical lines in contour
levels diagrams show the observational limits of the \met of the Hyades. {\it Solid
lines} isochrones in the CMD correspond to the best $\chi^2_{min}$ fits ({\it open
circles}, Z $=$ 0.027 and log t $=$ 8.80) and {\it dashed lines} isochrones correspond to the
{\it triangle} (Z $=$ 0.024 and log t $=$ 8.80, values from Perryman {\al} 1998 for the Hyades).
Another isochrone ({\it dot-dashed line}) corresponding to the {\it diamond} symbol
(Z $=$ 0.04 and log t $=$ 8.72) in the (t,Z) diagram is also shown in the Hipparcos CMD.
This solution is still an acceptable CMD fit at the 1$\sigma$ confidence level
even if the \met is twice solar,  which is excluded by observational constraints.}
\label{f:Theta02Tau}
\end{figure*}
The V818 Tau system (vB22) is a double-lined eclipsing binary (Mc Clure, 1982) with very
well estimated masses (actually the most accurate masses known for Hyades members).
Indeed, the relative errors on the masses are less than 1\%, and the secondary component
is particularly interesting because it is one of the rare stars which is less massive than
the Sun and whose mass is known with such high accuracy (cf. Andersen {\al} 1991). Unfortunately,
this low mass star (about 0.77 $M_{\odot}$) does not allow us to test either the CG92 models
-- the lower available mass of these models being 1 $M_{\odot}$ -- or the Geneva
models whose lower mass limit is 0.8 $M_{\odot}$. Nevertheless, we have tested Geneva
tracks (for the primary component) coupled\footnote{This simply means that the Geneva
tracks were extrapolated with the Baraffe {\al} models in the low mass region
(below 0.8 $M_{\odot}$) for each metallicity. Of course, this point is a very rough
approximation because the physics of these models are different, but it will not
change our final conclusions.}  with the  Baraffe {\al} (1995)
models (for the low-mass secondary star), as well as the Padova group models whose
lower mass limit is small enough for our purpose (0.6 $M_{\odot}$).\\
Torres {\al} [TSL97a] derived for this binary the distance d $=$ 50.4 $\pm$ 1.9 pc
indicating that V818 Tau is slightly more distant than the cluster center.
By using the Hipparcos parallax, we obtain d $=$ $46.7^{+2.9}_{-2.6}$ pc,
which seems to be in a better agreement with the distance of the Hyades center.
The confidence levels that we obtain by combining pre-Hipparcos data (see {\it upper panels}
in Fig. \ref{f:V818Tau}) and the isochrone fitting technique with the Padova tracks in
order to match simultaneously the locations of the two stars in the CMD, are in a
clear disagreement with the observational constraints of the Hyades metallicity.
As a matter of fact, the Padova as well as the Geneva tracks
predict metallicities much larger than expected from observational determinations:
1.5 to 2 times solar metallicities (Z$\in$[0.03,0.04]) provide the best fits as shown
in the {\it upper panels} of Fig. \ref{f:V818Tau}. The Padova isochrone corresponding to the
metallicity--age Hyades solution of the detailed work of Perryman {\al} (1998) is
also shown ({\it dashed line} in the upper CMD of  Fig. \ref{f:V818Tau}). This solution should
be consistent with the observational \met of the Hyades, however, the fit is clearly
bad in the CMD.\\
Now, if we consider the Hipparcos parallax of this binary system, the absolute
magnitude (see in particular the primary component, which puts the more stringent
constraints) is shifted towards fainter magnitudes, giving rise to significantly different
$\chi^2$-contours (see confidence contours in the {\it lower panel} of Fig. \ref{f:V818Tau}).
Hipparcos parallaxes have a strong influence on the shape of the isocontours
that we obtain: for instance, 1$\sigma$ confidence levels occupy a larger region with
Hipparcos and are in a better agreement with the observational constraints
({\it vertical lines} in the Z-t diagram).
We wish to emphazise that even if the best displayed Z-value inferred from Hipparcos
({\it open circle} in the {\it bottom panel} of Fig. \ref{f:V818Tau}) is actually the same as with
Torres {\al} (1997) (Z $\simeq$ 0.033), it is worth noticing that the Hipparcos parallaxes give also
possible solutions at 1$\sigma$ level with metallicities and ages lower than in the
pre-Hipparcos Z--t diagram ({\it left upper panel}) where solutions are confined in a
region roughly defined by Z $\geq$ 0.024 if log t $\geq$ 9.7, and Z $\geq$ 0.037 if
log t $\geq$ 9.
Therefore, if one considers the confidence levels, the disagreement found using orbital
parallaxes disappears, and the models do not fail anymore.
We would like to mention the fact that this result is rather puzzling because
the orbital parallaxes are a little more accurate than the Hipparcos parallaxes, that
is why such variation was not expected. The change of shape is due to the fact that
the distance derived from Hipparcos for V818 Tau is about 8\% smaller than from its
orbital parallax. The better consistency between the contours diagram of the Hipparcos
solution and the \met of the Hyades, which is the only reliable
constraint, gives more weight to the Hipparcos distance than to the orbital parallax.
This example highlights the importance of having very accurate but also reliable
fundamental data, because small errors on the data can lead to reject -- by
mistake -- the validity of a stellar model. \\
As mentioned in the beginning of this section, the masses of the two components of V818 Tau
are known with an excellent accuracy (better than 1\%, following the study of Peterson
\& Solensky, 1988, [PS88]). Therefore, to check that the
stellar masses predicted by the models are in agreement with the true masses is
probably the most critical test. A comparison is given in Table 4.
The result is that the best Padova fit underestimates
the masses of V818 Tau by about 5$\sigma$ for both stars. This is not so bad because
of the high level of accuracy of the masses: 5$\sigma$ only means 0.05$M_{\odot}$
for V818 Tau A and 0.025$M_{\odot}$ for V818 Tau B. \\
\begin{table}[htb]
\caption[]{Comparison of theoretical mass estimates from Padova isochrone age fitting
of the system V818 Tau with the values of [SM87] (Schiller \& Milone, 1987) and [PS88]
(Peterson \& Solensky, 1988).}
\begin{flushleft}
\begin{center}
\begin{tabular}{cccc}
\hline\noalign{\smallskip}
  & [SM87] & [PS88]  & Padova$^{a}$ \\
\noalign{\smallskip}
\hline\noalign{\smallskip}
\noalign{\smallskip}
A & 1.080$\pm$0.017 & 1.072$\pm$0.010 & 1.020$\pm$0.04  \\
B & 0.771$\pm$0.011 & 0.769$\pm$0.005 & 0.744$\pm$0.02  \\
\noalign{\smallskip}\hline
\end{tabular}
\end{center}
\smallskip
$^{a}$ 1$\sigma$ interval (this work). \\
\end{flushleft}
\end{table}
Moreover, since V818 Tau is a double-lined eclipsing binary, the radius of each component
is also known with an excellent accuracy (better than 2\%). The stellar radius can also be
computed from the effective temperature and the luminosity given by the Padova models.
Therefore, it is possible to compare the stellar radii predicted by the models with the true
radii. Unfortunately, even if Padova models predict a correct mass for each component
of V818 Tau, it appears clearly from Fig. \ref{f:V818_mr} that there is no Padova isochrone able
to fit both components of V818 Tau in the mass-radius diagram. Even with the best fit isochrone
obtained from the CMD of Fig. 3, the radius of the more massive component is overestimated
by more than 0.3 $R_{\odot}$, and the radius of the less massive component is underestimated
by more than 0.3 $R_{\odot}$.
This test shows that masses are much less discriminant, as far as the power of the test is
concerned, than radii, hence the importance of double-lined eclipsing binaries to fully
constrain stellar tracks.

\subsection{Results for $\theta^2$ Tau}

The primary component of the spectroscopic binary $\theta^2$ Tau (spectral type A7 III) is
one of the brightest stars in the Hyades.
Such a system is {\it a priori} very critical because it is composed by a main-sequence star
and an  evolved star, which allows us to test widely different evolutionary stages.
The tests that we performed with this binary are shown in Fig. \ref{f:Theta02Tau}
where the locations in the CMD are from Torres {\al} [TSL97c], except in the
{\it bottom panel} where the absolute magnitude $M_V$ is derived from the Hipparcos
parallax. \\
The first point is that the Hipparcos mission parallax has hardly an influence
on the luminosity of the two components. Therefore, the 1, 2 and 3$\sigma$ $\chi^2$-contour
levels show no real significant differences. Moreover, the best fits obtained in
Fig. \ref{f:Theta02Tau} present a very similar age and metallicity, putting the most massive
component at the end of the core hydrogen burning phase as pointed out by Torres {\al}
[TSL97c]. Nevertheless, if one believes a \met slightly poorer (for instance the solution
shown as a triangle symbol in the {\it lower panel} of Fig. \ref{f:Theta02Tau}) -- more in
agreement with the Hyades \met and still acceptable inside the 1$\sigma$-contour levels --
then this massive star could already be on the begining of the hydrogen-shell burning phase. \\
It is also worth noticing that both components of $\theta^2$ Tau (also known as 78 Tau)
are fast rotators. The primary component has v $\sin$ i $\simeq$ 80 \kms
(Slettebak {\al} 1975) and the secondary seems to rotate even faster (estimations range
from 90 to 170 \kms). Therefore, the rotational effect on their  locations
in the CMD  should certainly not be neglected. The effect expected is typically a few
tenths of magnitude in absolute magnitude and a few hundredths of magnitude in B$-$V, but
these values are highly dependent of spectral type, age, and chemical composition (see for
instance Maeder 1971 and Zorec 1992). As a direct consequence, this effect could modify the
results presented in Fig. \ref{f:Theta02Tau} because they are inferred from theoretical
tracks which neglect the stellar rotation effect. However, a detailed study of this point
is beyond the scope of this paper (and will be developed in a forthcoming paper). \\
Nevertheless, in the particular case of $\theta^2$ Tau, the stellar rotation effect
should not call into question the validity of the theoretical tracks of Geneva, Padova
or CG92, because the contours show a large range of possible \met (isocontours derived
from Padova models have the same shape/are identical than those of Geneva, as well
as the CG92 models whose upper limit is Z$=$0.03). Then, even with slight variations of
magnitude and colour in the CMD, a part of these $\chi^2$-contours will always be
in agreement with the observed \met contraints. \\
\begin{table}[htb]
\caption[]{Comparison of theoretical mass estimates from Geneva isochrone age fitting
of the system $\theta^2$ Tau with the values of [TPM95] (Tomkin {\al}, 1995)
and [TSL97c] (Torres {\al}, 1997).}
\begin{flushleft}
\begin{center}
\begin{tabular}{cccc}
\hline\noalign{\smallskip}
  & [TPM95] & [TSL97c]  & Geneva$^{a}$ \\
\noalign{\smallskip}
\hline\noalign{\smallskip}
\noalign{\smallskip}
A & 2.1$\pm$0.3 & 2.42$\pm$0.30 & 2.37$\pm$0.02  \\
B & 1.6$\pm$0.2 & 2.11$\pm$0.17 & 1.95$^{+0.06}_{-0.03}$  \\
\noalign{\smallskip}\hline
\end{tabular}
\end{center}
\smallskip
$^{a}$ 1$\sigma$ interval (this work). \\
\end{flushleft}
\end{table}
Since the masses of the two components of $\theta^2$ Tau are known to a good accuracy
(respectively 12\% and 8\%), to check that the predicted masses are in
agreement with the measured masses is one more stringent test.
Torres {\al} [TSL97c] updated the previous work on this system (Tomkin {\al} 1995),
which resulted in an increase of the masses ($M_A$ $=$ 2.42 $\pm$ 0.30 $M_{\odot}$ instead of
$M_A$ $=$ 2.10 $\pm$ 0.60 $M_{\odot}$ and $M_B$ $=$ 2.11 $\pm$ 0.17 $M_{\odot}$ instead of
$M_B$ $=$ 1.60 $\pm$ 0.40 $M_{\odot}$).
As shown in Table 5, the best Geneva fit gives a quite
good agreement  which means that these models are able to reproduce to a satisfying
level the stellar masses in the mass range of $\theta^2$ Tau. \\
The general conclusion of the study performed with $\theta^2$ Tau is that the three
theoretical models allow us  to fit correctly the system for (metallicity, age)-pairs
in agreement with the more recent constraints available about the \met of the Hyades
cluster.

\subsection{The influence of the Hipparcos parallaxes on the Hyades mass-M$_V$ relation}

\begin{figure*}[htb]
\centerline{\psfig{figure=ml.ps,height=11.truecm,rheight=11.5truecm,angle=-90.}}
\caption{Influence of the Hipparcos parallaxes on the Hyades mass-M$_V$
relation of the 6 stars studied in the present work. The components of
each  binary system are
connected by {\it dotted lines} and the Sun is also shown for comparison
(M$_V$$=$4.83 from Bessell 1991). On the {\it right panel}, V818 Tau ({\it square}),
51 Tau ({\it circle}) and $\theta^2$ Tau ({\it triangle}) are displayed on
a mass-$\Delta$M$_V$ diagram, where $\Delta$M$_V$ means M$_V$ from Hipparcos
parallaxes minus M$_V$ from orbital parallaxes. The $\Delta$M$_V$$=$0 line
({\it dotted line}) is shown for comparison.}
\label{f:ml}
\end{figure*}
The discussion of the empirical mass-luminosity relation of the Hyades is beyond
the scope of this work, because we only studied a tiny sample of member stars
(see Torres {\al} 1997 [TSL97a,b,c] for a critical and detailed discussion). However, it is
interesting to show the influence of the Hipparcos parallaxes on the
location of our working sample in a mass-luminosity diagram.
As it is only the influence of Hipparcos that is under scrutiny,  one can
conclude from Fig. \ref{f:ml} ({\it left panel}) that the global shape of this
empirical relation does not change. Actually, such a result was expected because
of the excellent accuracy of the orbital parallaxes obtained before Hipparcos,
but it was important to check this point.
Thus, the difference, $\Delta$M$_V$ (M$_V$ from Hipparcos parallaxes minus
M$_V$ from orbital parallaxes) is always smaller than 0.2 mag. and the error bars
show a very good agreement with $\Delta$M$_V$$=$0 (Fig. \ref{f:ml}, {\it right panel}). \\

\section{Conclusion}

The stellar theoretical models and tracks from Geneva, Padova and CG92 have been tested
with well-detached binary systems in the Hyades open cluster: 51 Tau, V818 Tau,
and $\theta^2$ Tau. Firstly, for each of the 3 selected systems, we computed
simultaneous metallicity-age solutions to fit the two components in the CMD
(a summary of the results is given in Table 6, taking into account the Hipparcos parallax).
These results are shown in confidence regions in the (Z,t)-plane.
Under the reasonable assumption that the metallicity must be the same and equal
to the Hyades \met for the 6 components, we had one more constraint, seldomly available
for field binaries. Moreover, the new Hipparcos parallaxes that we found for these
systems allowed us to put more weight on the power of the test. \\
\begin{table*}[htb] \caption[]{Summary of the theoretical simultaneous metallicity--age estimates
obtained from isochrone age fitting (1$\sigma$ level, this work) taking into account the Hipparcos
parallax.}
\begin{flushleft}
\begin{center}
\begin{tabular}{lllllll}
\hline\noalign{\smallskip}
System         & \multicolumn{2}{c}{Geneva} & \multicolumn{2}{c}{Padova} & \multicolumn{2}{c}{CG92} \\
\noalign{\smallskip}
\hline\noalign{\smallskip}
               & Z & log t                  & Z & log t                   & Z & log t               \\
\noalign{\smallskip} \hline\noalign{\smallskip}
\noalign{\smallskip}
51 Tau         & 0.020$^{+0.010}_{-0.008}$ & 8.88$^{+0.22}_{-0.23}$ &
0.017$^{+0.021}_{-0.005}$ & 8.90$^{+0.15}_{-0.55}$ &
0.018$^{+0.012}_{-0.006}$ & 8.92$^{+0.23}_{-0.17}$ \\
\noalign{\smallskip}
V818 Tau$^{a}$ &                           &                        &
0.033$^{+0.017}_{-0.015}$ & 7.30$^{+2.50}_{-0.30}$ &
                          &                        \\
\noalign{\smallskip}
$\theta^2$ Tau & 0.027$^{+0.013}_{-0.010}$ & 8.80$^{+0.05}_{-0.09}$ &
0.027$^{+0.023}_{-0.011}$ & 8.80$^{+0.03}_{-0.11}$ &
0.027$^{+0.003}_{-0.005}$ & 8.88$^{+0.02}_{-0.02}$ \\
\noalign{\smallskip}\hline \noalign{\smallskip} \end{tabular}
\end{center}
\smallskip
$^{a}$ As explained in Sect.3.2, the Geneva and CG92 models can not be tested with
the less massive component of V818 Tau.
\end{flushleft}
\end{table*}
The results of these tests are very satisfying for the 3 sets of tracks, except
for the case of V818 Tau if we used the orbital parallax (unfortunately, the CG92
and Geneva models can not be tested with the V818 Tau data because the mass of the
secondary is not in the proper range).
As shown by the 1$\sigma$ confidence levels, the Padova tracks predict a slightly
too rich \met for the V818 Tau members. The Geneva models also predict a larger \met
but we wish to emphazise the fact that in this particular case the test
does not have the same pertinence because we combined the Geneva with the Baraffe
{\al} (1995) models in order to be able to fit the low mass secondary component of
V818 Tau. Nevertheless, even if the best $\chi^2$-fit still gives a too
large metallicity (reported as the central value in Tab. 6: Z$\simeq$0.033) with Hipparcos,
the inconsistency with the Hyades \met disappears as soon as we use the Hipparcos parallax,
because the 1$\sigma$ confidence levels are in agreement with the \met constraints.\\
We also present some comparisons between the masses predicted by the models and
the true stellar masses which give more weight to the quality of the models. \\
Nevertheless, although the Padova models predict a correct mass for each component
of V818 Tau, there is no Padova isochrone able to fit both components of V818 Tau
in the mass-radius diagram. \\
As explained above, these tests are not completely unambiguous because
of the inherent problem of calibration between colour and effective temperature.
However we do not expect significant errors due to the photometric transformations
because we use the reliable transformations from the BaSeL models in the well known
Johnson photometric system and also because no disagreement exists
in the range of (B$-$V) colour relevant for the present study, for a \met close to solar.
Finally, for illustration purposes, we also present the influence of the Hipparcos
parallaxes on the empirical mass-luminosity relation existing for these 6 stars.

\begin{acknowledgements}
  E.L. thanks F. Genova (Director, CDS, Strasbourg Observatory) for useful suggestions
  on a preliminary version of this work and J. Fernandes for his comments.
  We acknowledge an anonymous referee for helpful suggestions which have
  improved the clarity of this paper.
  E.L. acknowledges support from the CDS
  and PPARC under the QMW Astronomy research Grant ZIB3.
  T.L. gratefully acknowledges support through the Swiss National Science
  Foundation (grant 20-53660.98 to Prof. R. Buser).
  This research has made use of the CDS resource facilities
  and the Simbad database operated at CDS, Strasbourg, France.
\end{acknowledgements}

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text:
URI Founder Speaks at TEDxSoMa
4 February 2019, 11:34 AM
URI Founder Bishop Swing delivers a "TED Talk" in San Francisco.
On January 15, 2019, TEDxSoMa brought together a group of esteemed visionaries at Yerba Buena Center for the Arts in San Francisco, CA, USA to "share new ideas that will shape our future together." The Right Rev. William Swing joined six other inspirational speakers to deliver talks about "masculinity, religion, mindfulness in policing, the hierarchy of language, facts vs. truth, and more." The theme was "Modern Campfires."
About Bishop Swing:
The Right Rev. William Swing is the President and Founding Trustee of United Religions Initiative (URI). The idea for URI came to Bishop Swing in 1993 after an invitation by the United Nations to host a large interfaith service in San Francisco, marking the 50th anniversary of the signing of the U.N. Charter. URI now has over 955 Cooperation Circles in 108 countries. Bishop Swing served as the Episcopal Bishop of California from 1980 until his retirement in 2006. In that capacity, he led the international Anglican response to the AIDS crisis, co-founded Episcopal Community Services to address San Francisco's homeless problem, and co-founded Community Bank of the Bay.
Bishop Swing is the author and co-author of several books, including The Sacred and the Silly: A Bishop's Playful and Eventful Life; A Bishop's Quest: Founding a United Religions; The Coming United Religions; co-author, Building Wisdom's House, and contributor to Andrei Sakharov, The Conscience of Humanity.
About TED Talks
TED is a nonprofit devoted to spreading ideas, usually in the form of short, powerful talks (18 minutes or less). TED began in 1984 as a conference where Technology, Entertainment and Design converged, and today covers almost all topics — from science to business to global issues — in more than 100 languages. TEDx brings the spirit of TED's mission of ideas worth spreading to local communities around the globe.
URI News Desk
The Rt. Rev. William E. Swing
President and Founding Trustee


text:
Mariusz Zbigniew Pudzianowski ps. Pudzian, Dominator, Pyton, Pudzilla (ur. 7 lutego 1977 w Białej Rawskiej) – polski zawodnik mieszanych sztuk walki (MMA), wcześniej utytułowany strongman i rugbysta. Obecny nr. 6 rankingu KSW w wadze ciężkiej.

Ośmiokrotny Mistrz Polski Strongman. Sześciokrotny Mistrz Europy Strongman w latach 2002–2004 i 2007–2009. Pięciokrotny Mistrz Świata Strongman w latach 2002, 2003, 2005, 2007 i 2008. Trzykrotny drużynowy Mistrz Świata Par Strongman w latach 2003–2005. Mistrz Super Serii w sezonach 2003/2004, 2005–2007. Zwycięzca i finalista wielu innych zawodów siłaczy.

Życiorys
Ma dwóch braci - Krystiana i starszego od siebie Dominika, którzy także są związani ze sportami siłowymi. Jest synem Marii Pudzianowskiej i sztangisty Wojciecha Pudzianowskiego, który był jego pierwszym trenerem sportów siłowych.

Rozpoczął treningi siłowe, będąc w szkole podstawowej. W wieku 16 lat wystartował w mistrzostwach Polski w wyciskaniu sztangi leżąc, jest czterokrotnym mistrzem Polski w tejże dyscyplinie. Trenował także karate kyokushin (obecnie posiada 4 kyu) oraz boks, jednak przed 11 grudnia 2009 nie stoczył żadnej oficjalnej walki. W międzyczasie pracował jako ochroniarz w patrolu interwencyjnym firmy Juwentus w Warszawie. Był również zawodnikiem rugby Budowlanych Łódź. Od 1999 r. był strongmanem.

W 2000 został skazany na karę 2,5 roku pozbawienia wolności za pobicie, po odbyciu 1 roku i 7 miesięcy kary uzyskał warunkowe przedterminowe zwolnienie.

Przed wyborami parlamentarnymi oraz prezydenckimi w 2005 brał udział w kampanii wyborczej Samoobrony RP i Andrzeja Leppera.

27 maja 2008 ukończył studia wyższe, uzyskując tytuł zawodowy licencjata w Społecznej Wyższej Szkoły Przedsiębiorczości i Zarządzania w Łodzi. Praca dyplomowa Mariusza Pudzianowskiego zatytułowana była Kultura organizacyjna w marketingu sportowym na świecie. 9 czerwca 2010 uzyskał tytuł magistra w Społecznej Wyższej Szkole Przedsiębiorczości i Zarządzania w Łodzi, uzyskując ocenę dobrą.

Mieszka pod Białą Rawską. Angażuje się również w różne przedsięwzięcia biznesowe; jest właścicielem firmy transportowej Pudzianowski Transport oraz Domu Weselnego w Białej Rawskiej.

Kariera strongmana

W zawodach Strongman zadebiutował 1 maja 1999 podczas konkursu w Płocku. Jest zrzeszony w światowej federacji siłaczy WSMC (The World Strongman Cup Federation).

Wraz z Jarosławem Dymkiem, na Drużynowych Mistrzostwach Świata Par Strongman 1999, zdobył reprezentując Polskę pierwszy w historii kraju medal w sporcie Strongman. Jest pierwszym i dotychczas jedynym Polakiem, który zdobył tytuł Najsilniejszego Człowieka Świata i pierwszym spoza USA i Europy Zachodniej, który zdobył ten tytuł.

W czasie pobytu w zakładzie karnym nie brał udziału w zawodach, m.in. nie mógł uczestniczyć w Mistrzostwach Europy Strongman 2001, Mistrzostwach Świata Strongman 2001 i Drużynowych Mistrzostwach Świata Par Strongman 2001.

Został Mistrzem Super Serii w sezonach 2003/2004, 2005, 2006 i 2007.

Wziął udział trzykrotnie w zawodach siłaczy Arnold Strongman Classic, rozgrywanych w Columbus (USA), w latach 2003, 2004 i 2006.

Od 2005 organizuje własny cykl dorocznych zawodów siłaczy zwanych Pojedynkiem Gigantów. Zawody rozgrywane są na początku roku w Łodzi.

Z powodu kontuzji (naderwanie bicepsu) nie mógł wziąć udziału w Mistrzostwach Polski Strongman 2005 i Mistrzostwach Europy Strongman 2005.

14 września 2008 na Mistrzostwach Świata Strongman 2008, pomimo kontuzji, zdobył kolejny tytuł Mistrza Świata Strongman i tym samym stał się pierwszym zawodnikiem posiadającym pięć tytułów Najsilniejszego Człowieka Świata.

Największym rywalem Pudzianowskiego na światowych arenach był Litwin, Žydrūnas Savickas, natomiast w obrębie własnej federacji Amerykanin, Derek Poundstone. Od połowy 2006 Pudzianowski nie dążył do pojedynku z Savickasem, a pierwsza sportowa konfrontacja nastąpiła na Mistrzostwach Świata Strongman 2009.

28 lutego 2009, podczas Piątego Pojedynku Gigantów, doznał zerwania bicepsu i w wyniku tej kontuzji został na kilka miesięcy wyłączony z zawodów.

Osiągnięcia jako strongman

 1999
 1. miejsce – Puchar Polski Strongman 1999 (pierwsza edycja Warka Strongman)
 3. miejsce – Drużynowe Mistrzostwa Świata Par Strongman 1999, Panyu, Chiny (z Jarosławem Dymkiem)
 2000
 1. miejsce – Puchar Świata
 1. miejsce – Mistrzostwa Polski Strongman 2000
 4. miejsce – Mistrzostwa Świata Strongman 2000, Sun City, RPA
 2. miejsce – Drużynowe Mistrzostwa Świata Par Strongman 2000, Węgry (z Jarosławem Dymkiem)
 2002
 3. miejsce – Drużynowe Mistrzostwa Świata Par Strongman 2002, Heerenveen, Holandia (z Jarosławem Dymkiem)
 1. miejsce – Mistrzostwa Europy Strongman 2002, Gdynia
 2. miejsce – Finał Pucharu Polski Strongman 2002, Ostrów Wielkopolski
 1. miejsce – Mistrzostwa Świata Strongman 2002, Kuala Lumpur, Malezja
 1. miejsce – Giganci Świata
 5. miejsce – Super Seria 2002: Sztokholm
 2. miejsce – Pierwsze zawody Polska kontra Reszta Świata
 2003
 3. miejsce – Super Seria 2003: Oahu
 1. miejsce – Super Seria 2003: Hawaje
 4. miejsce – Arnold Strongman Classic, Columbus, USA
 1. miejsce – Super Seria 2003: Silvonde
 1. miejsce – Mistrzostwa Polski Strongman 2003
 1. miejsce – Mistrzostwa Europy Strongman 2003, Sandomierz
 2. miejsce – Super Seria 2003: North Bay
 2. miejsce – Super Seria 2003: Imatra
 2. miejsce – Mistrzostwa World Muscle Power
 1. miejsce – Mistrzostwa Świata Strongman 2003, Wodospady Wiktorii, Zambia
 1. miejsce – World Record Breakers, Gdynia
 1. miejsce – Drużynowe Mistrzostwa Świata Par Strongman 2003, Węgry (z Jarosławem Dymkiem)
 1. miejsce – Finał Pucharu Polski Strongman 2003, Piła
 1. miejsce – Drugie zawody Polska kontra Reszta Świata
 2004
 5. miejsce – Arnold Strongman Classic, Columbus, USA
 1. miejsce – Finał Pucharu Polski Strongman 2004, Szczecin
 1. miejsce – Super Seria 2004: Moskwa
 1. miejsce – Mistrzostwa Polski Strongman 2004
 1. miejsce – Mistrzostwa Europy Strongman 2004, Jelenia Góra
 3. miejsce / dyskwalifikacja za doping – Mistrzostwa Świata Strongman 2004, Paradise Island, Bahamy
 1. miejsce – Drużynowe Mistrzostwa Świata Par Strongman 2004, Płock (z Jarosławem Dymkiem)
 1. miejsce – Polska – Skandynawia, Dąbrowa Górnicza
 2. miejsce – Pierwsze zawody Polska kontra Ukraina
 1. miejsce – Trzecie zawody Polska kontra Reszta Świata
 2005
 1. miejsce – Pierwszy Pojedynek Gigantów, Łódź
 1. miejsce – Drużynowe Mistrzostwa Świata Par Strongman 2005, Poznań (ze Sławomirem Toczkiem)
 1. miejsce – Super Seria 2005: Venice Beach
 1. miejsce – Super Seria 2005: Malbork
 1. miejsce – Super Seria 2005: Varberg
 1. miejsce – Puchar Świata Siłaczy 2005: Bad Häring
 1. miejsce – Super Seria 2005: Mohegan Sun
 1. miejsce – Finał Pucharu Polski Strongman 2005, Kielce
 2. miejsce – Zawody Północ-Południe, Darłowo
 1. miejsce – Mistrzostwa Świata Strongman 2005, Chengdu, Chiny
 1. miejsce – Czwarte zawody Polska kontra Reszta Świata
 2006
 1. miejsce – Drugi Pojedynek Gigantów, Łódź
 6. miejsce – Arnold Strongman Classic, Columbus, USA
 1. miejsce – Puchar Świata Siłaczy 2006: Ryga
 1. miejsce – Super Seria 2006: Mohegan Sun
 1. miejsce – Puchar Świata Siłaczy 2006: Mińsk
 1. miejsce – Super Seria 2006: Moskwa
 1. miejsce – Puchar Świata Siłaczy 2006: Moskwa
 1. miejsce – Super Seria 2006: Milicz
 1. miejsce – Mistrzostwa Polski Strongman 2006, Września
 2. miejsce – Mistrzostwa Świata Strongman 2006, Sanya, Chiny
 1. miejsce – Puchar Świata Siłaczy 2006: Grodzisk Mazowiecki
 1. miejsce – Puchar Świata Siłaczy 2006: Podolsk
 2007
 1. miejsce – Trzeci Pojedynek Gigantów, Łódź
 1. miejsce – Super Seria 2007: Mohegan Sun
 1. miejsce – Puchar Świata Siłaczy 2007: Ryga
 2. miejsce – Super Seria 2007: Venice Beach
 1. miejsce – Mistrzostwa Europy Strongman 2007, Łódź
 1. miejsce – Super Seria 2007: Viking Power Challenge, Storefjell
 1. miejsce – Puchar Świata Siłaczy 2007: Dartford
 1. miejsce – Puchar Europy Par Strongman WP 2007, Oleśnica (z Damianem Sierpowskim)
 1. miejsce – Puchar Polski Strongman 2007, Strzegom
 1. miejsce – Mistrzostwa Polski Strongman 2007, Strzegom
 1. miejsce – Mistrzostwa Świata Strongman 2007, Anaheim, USA
 2008
 2. miejsce – Super Seria 2008: Mohegan Sun
 1. miejsce – Czwarty Pojedynek Gigantów, Łódź
 1. miejsce – WSF Puchar Świata 2008: Irkuck
 1. miejsce – Polska kontra Europa, Cieszanów
 1. miejsce – Grand Prix Polski Strongman 2008, Radom
 1. miejsce – Finał Pucharu Polski Strongman 2008, Kołobrzeg
 1. miejsce – Mistrzostwa Europy Strongman 2008, Szczecinek
 1. miejsce – Mistrzostwa Polski Strongman 2008, Częstochowa
 1. miejsce – Mistrzostwa Świata Strongman 2008, Charleston (Wirginia Zachodnia), USA
 2009
 8. miejsce – Piąty Pojedynek Gigantów, Łódź (kontuzjowany)
 1. miejsce – Mistrzostwa Europy Strongman 2009, Bartoszyce
 1. miejsce – The Globe's Strongest Man, Grand Prix Moskwy
 1. miejsce – Mistrzostwa Polski Strongman 2009, Trzebiatów
 1. miejsce – Mistrzostwa Polski Strongman A-S 2009, Malbork
 1. miejsce – Mistrzostwa Polski Strongman w Parach 2009, Krotoszyn (z Januszem Kułagą)
 2. miejsce – Mistrzostwa Świata Strongman 2009, Malta
 1. miejsce – Halowy Puchar Polski Strongman 2009, Lębork
 2010
 1. miejsce – Halowy Puchar Polski Strongman 2010, Gdańsk

Rekordy

Strongman
 Spacer farmera – 100 m
 Spacer farmera 75 m na czas – 30,45 s
 Przerzucanie opony (sześć obrotów w jedną stronę bez dobiegu) – 10,87 s
 Konkurencja wiązana (worki + kowadło) – 20,81 s
 Spacer drwala – 98 m
 Spacer drwala z tarczą – 187,47 m
 Schody równoległe – 19,69 s
 Zegar – 1 380°

Trójbój siłowy
 Wyciskanie leżąc: 295 kg.
 Przysiad ze sztangą: 395 kg.
 Martwy ciąg: 415 kg.

Kariera MMA

Początków treningu i pierwsze zawodowe walki

Treningi MMA rozpoczął po zakończeniu kariery jako strongman, twierdząc, że "osiągnął już wszystko". Po wielu latach amatorskich treningów sportów walki, chciał spróbować swych sił w oficjalnym pojedynku. 11 grudnia 2009 na gali KSW 12, na warszawskim Torwarze stoczył debiutancką walkę w formule MMA z pięściarzem Marcinem Najmanem. Do walki przygotowywał go między innymi Mirosław Okniński i Piotr Kroczewski. Pudzianowski zapowiadał wykorzystanie swojego największego atutu, siły fizycznej i pokonanie rywala w parterze. Pudzian wygrał z Najmanem przez TKO w 43. sekundzie walki, wykorzystując niskie kopnięcia, a następnie uderzania pięściami w parterze.

7 maja 2010, podczas KSW XIII pokonał Japończyka Yūsuke Kawaguchi przez jednogłośną decyzję sędziów po dwurundowym pojedynku.

Walka w USA i nowy kontrakt z KSW
21 maja 2010 w Worcester w walce w ramach Moosin: God of Martial Arts przegrał przez poddanie na skutek ciosów w parterze z dwukrotnym mistrzem UFC, Timem Sylvią.

Cztery miesiące później, 18 września 2010, podczas gali KSW XIV pokonał przez poddanie ważącego ponad 80 kg więcej boksera Erica Escha.

W 2011 podpisał z KSW kontrakt na dwie kolejne walki. Pierwszą z nich stoczył 21 maja 2011 w Ergo Arenie, gdy przegrał przez poddanie z Brytyjczykiem Jamesem Thompsonem. We wrześniu wyjechał na treningi do USA, gdzie na Florydzie trenował w klubie mieszanych sztuk walki – American Top Team.

26 listopada na gali KSW 17, w walce rewanżowej z Jamesem Thompsonem, w wyniku pomyłki jednego z sędziów punktowych, doszło do błędnego ogłoszenia wygranej Polaka. Ostatecznie, walka została uznana za nieważną.

Od stycznia 2012 ponownie przebywał na Florydzie, gdzie trenował w klubie American Top Team. 12 maja 2012 wystąpił w walce wieczoru na gali KSW 19, podczas której pokonał Boba Sappa przez TKO w 1. rundzie. Wówczas jego waga wynosiła 123 kg.

2012-2015
Kolejną walkę stoczył 15 września 2012, na gali KSW 20. Pokonał w niej przez nokaut techniczny (ciosy pięściami) Christosa Piliafasa. 16 grudnia na gali MMC Fight Club miał zmierzyć się w Londynie z Tyberiuszem Kowalczykiem, który nominalnie miał stoczyć walkę w formule K-1 z Marcinem Najmanem, lecz Najman zrezygnował z pojedynku ze względu na "niewywiązanie się z ustaleń, organizatorów tej walki". Do walki z Pudzianowskim także nie doszło, ponieważ organizatorzy gali nie wywiązali się ze zobowiązań.

8 czerwca 2013 na KSW 23 przegrał przez poddanie w 1. rundzie z Seanem McCorkle. Po tej porażce zmienił częściowo sztab trenerski. Jego głównym trenerem został Piotr Jeleniewski. 28 września 2013 na KSW 24 w Łodzi zrewanżował się Seanowi McCorkle wygrywając z nim po dwóch rundach jednogłośną decyzją sędziów.

17 maja 2014 podczas pierwszej gali KSW, na której walki odbywały się w okrągłej klatce, wygrał przez jednogłośną decyzję sędziów z byłym strongmanem oraz zawodnikiem UFC Brytyjczykiem Olim Thompsonem.

6 grudnia 2014 zmierzył się z mistrzem olimpijskim w judo Pawłem Nastulą. Po dwóch rundach sędziowie ogłosili remis, natomiast podczas trzyminutowej dogrywki Pudzian, dominując byłego olimpijczyka, wygrał walkę.

25 maja 2015 w Gdańskiej Ergo Arenie wygrał przez widowiskowy nokaut z Rollesem Gracie w 27. sekundzie walki. Walka została uznana za nokaut wieczoru gali KSW 31.

Walka na pierwszej zagranicznej gali KSW i kariera do 2017
31 października 2015 podczas pierwszej zagranicznej gali federacji KSW w Londynie po serii czterech wygranych walk z rzędu, mimo dominacji w pierwszej rundzie, przegrał w drugiej minucie drugiej rundy z mistrzem Australii w wadze ciężkiej w boksie oraz legendą K-1 Australijczykiem Peterem Grahamem.

27 maja 2016 na gali KSW 35 przegrał w 1:46 sekundzie drugiej rundy z Marcinem Różalskim przez duszenie gilotynowe.

3 grudnia 2016 w Krakowskiej Tauron Arenie podczas KSW 37 Circus of Pain zwyciężył w 80. sekundzie walki w hitowym starciu z powracającym na ring Pawłem "Popkiem" Mikołajuwem.

27 maja 2017 podczas historycznej gali KSW 39 Colosseum zorganizowanej na Stadionie Narodowym w Warszawie przy publiczności ponad 56 tysięcy widzów wygrał przez poddanie z byłym strongmanem Tyberiuszem Kowalczykiem.

Niedoszła walka z McSweeneyem, eliminator do walki o pas
22 października 2017 podczas zagranicznej gali KSW 40 w Dublinie Mariusz Pudzianowski miał się zmierzyć z wywodzącym się z kickboxingu Jamesem McSweeneyem. Jednak ze względu na zablokowanie Anglika przez Irlandzką organizację zajmującą się zdrowiem zawodników SafeMMA Pudzianowski stoczył pojedynek ze znanym z trylogii z byłym mistrzem KSW Michałem Materlą, Jayem Silvą. Po widowiskowym starciu Pudzian wygrał walkę przez większościową decyzję sędziów.

9 czerwca 2018 podczas gali KSW 44 w ERGO Arenie w Gdańsku stoczył walkę z Karolem Bedorfem. Walka była eliminatorem do walki o mistrzostwo KSW w wadze ciężkiej. "Pudzian" przegrał w drugiej minucie pierwszej rundy przez poddanie (kimura).

23 marca 2019 na gali KSW 47: The X -Warriors przegrał w pierwszej rundzie z byłym sztangistą Szymonem Kołeckim przez kontuzję zerwania mięśnia dwugłowego uda.

Najdłuższa seria zwycięstw, kariera od 2022
9 listopada 2019 podczas gali KSW 51 w Chorwacji znokautował bośniackiego kulturystę Erko Juna w drugiej rundzie.

21 marca 2021 na gali KSW 59 w Łodzi znokautował serbskiego zawodnika judo i sambo, Nikole Milanovicia, którego była to debiutancka walka. Pierwotnie przeciwnikiem Pudziana miał być senegalski zapaśnik Serigne Ousmane Dia "Bombardier", który w dniu walki doznał ostrego ataku wyrostka robaczkowego i został hospitalizowany.

5 czerwca 2021 podczas gali KSW 61: To Fight or Not To Fight w Gdańsku, w ERGO Arenie pokonał wieloletniego weterana oraz komentatora KSW – Łukasza Jurkowskiego przez techniczny nokaut w 3 rundzie.

24 października 2021 podczas wydarzenia KSW 64 doszło do pojedynku z Senegalskim Bombardierem. Walka zakończyła się przez błyskawiczny nokaut już po 18-stu sekundach, kiedy to Pudzian trafił rywala prawym prostym.

28 maja 2022 w walce wieczoru gali KSW 70 rękawice skrzyżował z czołowym zawodnikiem wagi średniej, Michałem Materlą. Walka zakończyła się przez nokaut już w pierwszej rundzie, po tym jak popularny Pudzian wystrzelił ciosem podbródkowym, gasząc światło zawodnikowi ze Szczecina. Starcie odbyło się w wadze ciężkiej. Po walce otrzymał drugi w karierze bonus za nokaut wieczoru.

17 grudnia 2022 podczas walki wieczoru XTB KSW 77, która odbyła się w Arenie Gliwice, zmierzył się z byłym mistrzem KSW w wadze półciężkiej (2009–2011) oraz średniej (2015–2018, 2020–2021), Mamedem Chalidowem. Do tej walki wyjątkowo nie przygotował go jego wieloletni trener, Arbi Szamajew, który ma bliskie relacje z Chalidowem. Pudzian przegrał przez techniczny nokaut w pierwszej rundzie, odklepując serię ciosów Chalidowa w parterze.

Lista zawodowych walk w MMA

Kariera muzyczna

Brat Mariusza Pudzianowskiego, Krystian, w 2005 założył zespół muzyczny Pudzian Band. Wspólnie nagrali teledysk do piosenki "Zdobyć świat", która promowała ich pierwszą płytę. Mariusz Pudzianowski wychodził do swoich walk w rytm piosenek wykonywanych przez brata, np. "Dawaj na ring".

Dyskografia

Teledyski
 "Dawaj na ring" (Pudzian Band)
 "Zdobyć Świat" (Pudzian Band)
 "Po prostu sobą bądź" (Pudzian Band)
 "Takich już nie ma" (A2)
 "Cała sala"
 "Czuję kiedy jesteś"

Programy telewizyjne
W 2003 roku wystąpił gościnnie w specjalnym odcinku programu "Twoja droga do gwiazd". Był uczestnikiem siódmej edycji programu rozrywkowego TVN Taniec z gwiazdami (2008) i pierwszego sezonu programu Polsatu Just the Two of Us. Tylko nas dwoje (2010); w obu konkursach zajął drugie miejsce w finale. Odrzucił także propozycję występu w programie Gwiazdy tańczą na lodzie. Był uczestnikiem programu TVP2 Przygarnij mnie (2016) i jurorem programu Polsatu The Brain. Genialny umysł (2017).

Filmografia
 2004: Na Wspólnej odc. 346, 358, 374 jako Przemas Zieliński, kolega Grzegorza Zięby
 2004: Dziki odc. 8 jako wynajęty zabójca
 2004: Camera Café odc. 53 (epizod 2) jako chłopak Beaty
 2005: Nie ma takiego numeru jako "Siłacz"
 2007: Faceci do wzięcia odc. 37 jako kulturysta w reklamie maszynki do golenia
 2007: Niania odc. 61 jako właściciel restauracji
 2008: Daleko od noszy odc. 166 jako Juliusz, miłość siostry Basen
 2014: Sąsiady jako wikary

Przypisy

Linki zewnętrzne
 oficjalna strona Mariusza Pudzianowskiego

 Mariusz Pudzianowski w bazie Sherdog
 Mariusz Pudzianowski w bazie Tapology

Absolwenci Społecznej Akademii Nauk w Łodzi
Ludzie urodzeni w Białej Rawskiej
Polscy przedsiębiorcy XXI wieku
Polscy sportowcy ukarani za doping
Polscy strongmani
Polscy zawodnicy MMA
Polscy zawodnicy rugby union
Rugbyści Budowlanych Łódź
Uczestnicy programów typu reality show
Osobowości telewizyjne związane z Polsatem
Urodzeni w 1977

redpajama_set_name: RedPajamaWikipedia


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text:
Rudo Mhonderwa (born 9 September 1995) is a Zimbabwean long-distance runner. In 2019, she competed in the senior women's race at the 2019 IAAF World Cross Country Championships held in Aarhus, Denmark. She finished in 101st place.

In 2017, she competed in the senior women's race at the 2017 IAAF World Cross Country Championships held in Kampala, Uganda. She finished in 75th place.

References

External links

Living people
1995 births
Place of birth missing (living people)
Zimbabwean female long-distance runners
Zimbabwean female cross country runners


Join people around the world to leave your cars at home today.
Tomorrow is the first day of autumn, and what better time to ride a bike than in the fall? Try riding to the store or run your errands and enjoy the freedom without a car. Walking and public transportation are also great options for World Carfree Day. If you can't leave the car at home all of the time, going carlite can still have a positive impact on your life, the city you live in, and your climate.
If you go by bike today, and you are new to bike commuting, check out the League of American Bicyclists and Commute by Bike.