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Wellesley's P2P lending rates appear higher on its own website than on 4thWay®.
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Important information before you visit Wellesley & Co.
Wellesley & Co. is primarily a P2P lending website.
But, when you visit the Wellesley website, you'll see that it also offers "bonds". Unlike its P2P lending service, its bonds don't allow you to lend directly to 100+ borrowers.
Instead, you lend to Wellesley and it lends to other borrowers.
We have not risk-rated either of those bonds, but we expect that their structure makes them more risky, particularly because you're lending to just one borrower.
But, when you visit the Wellesley website, you'll see that it also offers two "bonds", one of which is available as an ISA.
Unlike its P2P lending service, neither of these bonds allows you to lend directly to 100+ borrowers.
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Orchard's lending rates appear higher on its own website than on 4thWay®.
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Thomas Phinney was born in the United States, but raised largely in Canada. After finishing an undergraduate degree in psychology and political science, he almost went into journalism, but instead pursued his passion for typography. He got an MS in typography and printing at the Rochester Institute of Technology in 1997. Thomas briefly taught font production and worked for a variety of clients, including Monotype, Apple and Microsoft, before joining Adobe's typographic staff in 1997. While at Adobe, he helped define the company's approach to implementing, testing and evangelizing OpenType fonts, and got an MBA from UC Berkeley. He left Adobe in 2008, and is now Vice President of FontLab, while consulting and teaching on the side, and is based in Portland, OR.


With recreation lands, beautiful views, world-class energy-generation exhibits and historic buildings, NYPA's three Visitors Centers have attracted millions to the grounds of our major hydroelectric power projects. Plan your visit to our family-friendly, admission-free Visitors Centers today.
Housed in a 19th-century dairy barn Blenheim-Gilboa features exhibits describing the unique engineering of a pumped-storage power facility. On the grounds stands Lansing Manor, an 18th century home preserved for modern visitors. Hiking, boating and fishing are very popular.
The Hawkins Point Visitors Center nests on an island in the St. Lawrence River. Visitors will learn about the series of dams, walls, and canals that let the enormous river provide power to both Canada and New York. The center's local events include pajama parties, a wildlife festival, free movie showings, ice cream socials and more.
At recently renovated Niagara Power Vista, the power generation exhibits are on a par with those of the best science museums in the country—and it's just five miles from Niagara Falls. The center hosts local events ranging from movie days during school vacation weeks to the annual Festival of Trees, a hall filled with trees decorated every which way.
Located in the west, in the north and in the east-central parts of the state, NYPA Visitors Centers are popular day trips.


LOS ANGELES — Derek Fisher sticks to the background most nights for the Los Angeles Lakers, contributing a few assists and an occasional 3-pointer while his high-profile teammates get all the attention.
Every once in a while, the old D-Fish comes out to remind the Lakers' potential playoff opponents there's a world-class closer lurking back there behind Kobe Bryant and Pau Gasol.
Fisher spearheaded a late comeback with big back-to-back defensive plays to put the Lakers ahead, followed by the clinching jumper with 10 seconds left in Los Angeles' 12th win in 13 games since the All-Star break, 84-80 over the Portland Trail Blazers on Sunday night.
Bryant scored 10 of his 22 points in a dynamic fourth quarter for the Lakers, who won their first game without suspended center Andrew Bynum. Fisher had early foul trouble and scored just eight points, but he took over late.
Moments after feeding Bryant for a tying dunk, Fisher's steal and layup with 1:56 to play gave Los Angeles its first lead since the first half. His icy-cool 17-footer wrapped up the Lakers' remarkable rally.
Although their last two wins haven't exactly been works of art, the Lakers formally clinched a playoff berth earlier Sunday when the Utah Jazz lost to Houston. The win also wrapped up their fourth consecutive Pacific Division title and 50-victory season.
Bryant thrived again despite his sprained ankle and sore jaw, highlighting his night with a picture-perfect fallaway jumper with 32 seconds to play. Gasol added 14 points and 13 rebounds while taking on more work in the absence of Bynum, who was suspended two games by the NBA on Sunday for his flagrant foul on Minnesota's Michael Beasley two days earlier.
Nicolas Batum scored 22 of his 25 points in the first three quarters for the Blazers, whose three-game winning streak ended with a fourth-quarter flop, scoring just 14 points on 5-for-18 shooting.
LaMarcus Aldridge scored 18 points, and Marcus Camby grabbed 10 rebounds before hobbling off the court with an injured ankle in the final minutes. He'll have X-rays on Monday.
In Bynum's absence, Portland outrebounded the Lakers 45-35 — grabbing 17 offensive boards — and nursed a steady lead throughout the second half after making a 15-0 run spanning halftime, holding the Lakers without a field goal for 6 1/2 minutes.
But Bryant's acrobatic layup pulled Los Angeles to 74-72, and Bryant dunked after a turnover and a pass from Fisher to even it at 76 with 2:20 to play.
After Fisher's layup and a jumper by Bryant with 1:11 left put the Lakers up by four points, Ron Artest got a technical foul from referee Dan Crawford after exchanging shoves down low with Gerald Wallace. Bryant and Fisher calmly replied with late jumpers.
Bryant showed no ill effects early from his sprained ankle and a sore jaw resulting from a head-to-head collision with Minnesota's Martell Webster. The All-Star game MVP scored 10 points in the first half, but the Lakers missed Bynum's defensive presence and even his scoring in the first half, getting just eight points apiece from Gasol and Odom.
Portland took its first lead on Aldridge's layup 53 seconds before halftime. Batum went 8 for 10 for 19 points in the first half, hitting a 3-pointer in the final minute to stake the Blazers to a 48-44 lead.
Matt Barnes banked in a 3-pointer from a step inside the half-court line at the third-quarter buzzer, trimming the Blazers' lead to 66-62.
With three straight losses to the Lakers, Portland lost the season series with Los Angeles for the first time since 2004-05. … The Lakers have reached the playoffs in 33 of the last 35 seasons, missing the postseason only in 1993-94 and 2004-05. … Fans near courtside included Bruce Willis, Will Ferrell, David Arquette and Andy Garcia.
This video was posted in Highlights and tagged Los Angeles Lakers, Portland Trail Blazers. Bookmark the permalink.


The Bacardi Cocktail Drink Recipe is an intoxicating beverage. It is a colorless alcoholic liquor which was originally distilled a fermented cane product such as molasses or sugar cane. Made in a variety of countries in a clear (white) or dark color but is especially associated with the Caribbean.
Serve your classic Bacardi Cocktail speciality recipe in unusually shaped drinking glasses. Give your drinking glasses a frosted edge by dipping the rim into Lemon juice and then dipping it into sugar. Simple but effective drinking glasses! Put the drinking glasses on colorful drink coasters.
Rum based Bacardi Cocktail from an easy to make recipe!


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Terror Attack at New Zealand Mosques 49 Dead, 3 Arrested
by Mckenzie Santa Maria
New Zealand is mourning after 49 people were killed and over a dozen were injured in shootings at two mosques. Prime Minister Jacinda Arern announced holding back tears, that "gun laws will change. "Although documents state, the suspect had a license to carry the types of guns used in deadly attacks.
According to the announcement given during a press release broadcasted around the world, investigators who first arrived at the scene found five guns that were used by the main suspect which included, two semi-automatic weapons, two shotguns, and a lever-action firearm.
Police have reported that they have arrested three people. One Australian national man in his late 20s, whom the authorities declined to name, was charged with murder and was required in court on Saturday morning.
The New Zealand prime minister has called the attack an act of terrorism that resulted in "one of New Zealand's darkest days." Seventeen minutes of the live video appeared on Facebook that shows cased the horrible slaughter of innocent people on sites like Facebook, Twitter, and YouTube, concerning many about the role social media plays in radicalization.
Authorities are also investigating a 74-page manifesto that has been left after the shooting that disgraced Muslims and immigrants and cites multiple right-wing extremists who have committed violent acts of terror.
During a six-minute period of video that was streamed throughout multiple media sites, the man, dress head to toe in tactical gear and a camera attached to his vest shot hundreds of rounds into dozens of people. Many who appeared to be huddled together defenselessly against the walls of the mosque's main room, while others attempted to flee as shots rang off rapidly in every direction.
Details that defined this as a terrorist attack include the fact that his weapon had neo-Nazi symbols and multiple names of white right-wing extremist who have also committed acts of terror killing hundreds because of their ethnicity or faith. The manifesto released by New Zealand authorities outlines his motives that led to killing Muslim immigrants. Seven other people were shot to death at another mosque nearby, bringing the toll of the two attacked to 49 deaths.
Three people have been arrested in connection with the shooting. The 28- year who is accused of being the mastermind behind the plan is said to appear in court to face murder charges. The others are still being investigated on what their true connections were, "to establish whether the other two who were arrested were directly involved with this incident."
"This individual has traveled around the world, with sporadic periods spent in New Zealand," Ardern said, noting that the suspect was based in Dunedin, New Zealand, at the time of the attack.
The cruel act that has saddened a country brings consequences across the globe, the President of the United States, President Trump has voiced his opinion agreeing with the Prime Minister that this is, in fact, an act of terrorism.
Gun laws and other controversial questions have abruptly surfaced. The investigation is still ongoing.
If someone is looking for treatment for prescription drug abuse or mental illness close to home, search "Drug Rehab "and use the directory to find a center. For more information, please call our 24-hour hotline, CALL (888) 510-3898
The Recover is an unbiased substance abuse and mental health news provider. Helping individuals looking for the right treatment programs in their area. Also providing information on drug rehab centers for addiction recovery.
Contact: McKenzie Santa Maria
Company: The Recover
Address: Huntington Beach, CA
Website: www.therecover.com
Co-Founder of Self-Help Group Likely to Plead Guilty in Sex Slave Case, New Charges Surface
A Universal Basic Income Program Is Set To Be Tested By New Jersey's Largest City

redpajama_set_name: RedPajamaCommonCrawl


# Details: I had come across a female called Svetlana on the site Russian Euro(ID No.1004799) about 15 months back. After exchanging a few mails with her i stopped going on that site and began an exclusive correspondence with her. She never told me her surname or asked for money via e-mail or phone calls that i made to her(she never called). I had checked up her phone number and e-mail id and photos on Jim anti-scam site but did not find them.She wrote things that made it appear that she was interested in pursuing a serious relationship. When i visited her in February, she told me it is better to stay in an apartment than hotel at same price(see mail below) and said she can help me to rent one. Once i reached the apartment she and her mother forced me to pay 1 and half times the normal price and insisted on all of it being paid at once and gave me no receipt. Also they were reluctant to introduce me to the owner.rnShe met me for 3 days after this and began taking me to expensive hotels and enjoying good food at my expense. She claimed her salary was only 200 USD per month and began asking me money for passport (300 USD),english lessons (150 USD), wanted me to buy her shoes etc. I did not pay her. I could see that she came to me only at lunch time for about an hour and feigned interest in me. She also ordered extra food and took it with her as parcel. She was trying to hide her meetings with me from her friends and never showed me where she lived or worked even though she claimed to work nearby.rnI asked some local persons to carry out a background check on her. They told me that she has a local boyfriend with whom she has a serious relationship and she is trying to cheat me just like how she has cheated other foreigners before. I told her that i will call the police if she did not refund the excess money for the apartment. So she made a false complaint with the police that i was threatening her and came with 2 men who claimed to be police on the night before my departure. They claimed that i should settle this amicably or else they will imprison me. So i was forced to back out as they took her side and threatened to implicate me in a false scam. They spoke in Russian among themselves.rn Foll. is the information she gave me during the initial 2 days:rnName: Svetlana KovalevarnMothers name: Marina(First she claimed her mother is a physician and later claimed that she is nurse)rnFathers name:SergeirnDate of birth : 5th May 1989rnGraduated from Agrarian University as technologist (meat products). She now claims to work in a beauty saloon on Sovietskaya street, Lugansk as she cant find work as technologist.rnParents are divorced. Claims father left them for another woman. Her mother is involved in the scam as both came to pick me up at the airport and gave me a hefty taxi bill. They insisted on my paying them and claimed they will give it to the taxi driver as it was dark in that place at night, i had no choice. Dont know if her boyfriend is involved.rnrnI have seen that she keeps 2 phones. One of the phone numbers ( used to communicate with me ) is +380686918109rn The reason for this mail is that i do not want others to go through what i went.rnrn--- On Mon, 30/1/12, Tiramisu07 wrote:rnrnFrom: Tiramisu07 rnSubject: SvetarnTo: "D Fernandes" rnDate: Monday, 30 January, 2012, 7:58 AMrnrn Hello dear Dan!!!rnThank you for message,I will wait your information!!!rnDear,dont worry,I meet you in airport if you tell me when you come to Donesk:))rnYou want live in hotel or apartment???rnHere many hotels,for example "Lugansk","Druzba","Sovietskaya" and more others!!rnBut I think that in apartment will more comfortable and the same price!!!rnOk,let me know what you think about it.rnHave a nice day,kiss you,Sveta.


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Q: UIScrollView not bouncing vertical when scrolled to top i have a weird issue with a UIScrollView and a UIWebView in it.
First my setup:
I subclassed a UIView and added the following code to it:

.h
@interface MySubclassedView : UIView {
    UIScrollView *scrollView;
    UIWebView *contentView;
}

@property(nonatomic,retain) UIWebView *contentView;

.m
- (id)initWithFrame:(CGRect)frame {
    self = [super initWithFrame:frame];
    if (self) {
        self.autoresizingMask = UIViewAutoresizingFlexibleWidth | UIViewAutoresizingFlexibleHeight;
        [self setupContentView];
    }
    return self;
}

setupContentView
-(void)setupContentView {

    // Content View
    self.contentView = [[UIWebView alloc] init];
    self.contentView.backgroundColor = [UIColor whiteColor];

    // ScrollView
    scrollView = [[UIScrollView alloc] init];
    scrollView.backgroundColor = [UIColor whiteColor];
    scrollView.alwaysBounceVertical = YES;
    [scrollView addSubview:self.contentView];
    [self addSubview:scrollView];
}

and my layoutSubViews
- (void)layoutSubviews {
    XLog(""); // something like NSLog
    [super layoutSubviews];
    scrollView.frame = CGRectMake(0,0, self.width, self.height);
    self.contentView.frame = CGRectMake(0,0, self.width, self.height);
}

The Problem with all of this is, that it bounces the first time when my scrollview is not completely scrolled to the top. after the scrollview is scrolled to top or bottom i cannot drag the view downwards but the layoutSubviews method gets called on and on as long as i'm dragging.
For better understanding i made a short screen video to demonstrate the behavior: http://www.screenr.com/Gy9
thanks for all help. if something is unclear, please let me know in the comments.

A: I'm really sorry I don't have something more helpful, but:

Important: You should not embed
  UIWebView or UITableView objects in
  UIScrollView objects. If you do so,
  unexpected behavior can result because
  touch events for the two objects can
  be mixed up and wrongly handled.

from:
http://developer.apple.com/library/ios/#documentation/uikit/reference/UIWebView_Class/Reference/Reference.html
Doesn't mean there's no way to make it work. But probably means you want to limit the amount of time you spend banging your head against the wall trying to get it to work.
That said, I have successfully embedded UIWebViews in UIScrollViews as long as one's userInteractionEnabled was set to NO.

redpajama_set_name: RedPajamaStackExchange


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Gogoro's first e-bike is coming to the US next month
Eeyo electric bikes are then heading to Europe and Taiwan this summer
By Thomas Ricker@Trixxy Apr 23, 2020, 4:59am EDT
Share All sharing options for: Gogoro's first e-bike is coming to the US next month
Eeyo is the new Gogoro e-bike brand.
Image: Gogoro
Electric scooter company Gogoro, founded by two former senior HTC designers and technologists, is about to launch its first electric bike under the new Eeyo sub-brand. It's coming first to the US in May, before heading to Europe and the company's home country of Taiwan sometime in the summer.
Unfortunately, that's all we know right now, thanks to a teaser posted to Instagram and Twitter. But given the company's history, our expectations are high.
Gogoro made a big splash with the launch of its first Smartscooter in 2015. The technologically advanced scooter not only looked great, it also featured an innovative battery-swap subscription service and an app that allowed you to personalize your ride. Gogogo riders simply pull up to any 24/7 GoStation to replace their depleted batteries in seconds. The company has since produced a variety of scooter designs that brought a touch of fun and style to two-wheeled culture in scooter-obsessed Taipei and beyond.
A new ebike from @WeAreGogoro. Coming to the US in May. Europe and Taiwan this summer. Prepare for liftoff. pic.twitter.com/XscK7str1b
— Gogoro Eeyo (@eeyobike) April 22, 2020
What does that tell us about the new Gogoro Eeyo e-bike? Well, nothing is certain, but Gogoro scooters are already steeped in tech found on premium e-bikes. Some examples include firmware-upgradable onboard computers, anti-theft systems like automatic locking and unlocking that use proximity or biometric keys, scratch-resistant finishes, integrated hub motors, Gates carbon belt drives, Panasonic battery cells, and hydraulic disc brakes. The company also had a longstanding relationship with Bosch.
Now is certainly a great time to buy an e-bike, assuming you can still afford one amid skyrocketing unemployment and financial uncertainty. With pandemic-stricken cities eager to get back to work in lieu of a vaccine, e-bikes are becoming more attractive alternatives for commuters hoping to avoid public transportation, keep the air clean, and exercise those lungs in the process.


Puzzle round 2, Four Winds / Eight Winds - does every cell in the grid have to be used?
Puzzle round 5, Pento Coral - must the pentominoes completely cover the coral i.e. must it consist of exactly 55 shaded squares?
In the instructions for Trio Cut, should the word "tetrominos" be replaced by "triominos" or is it triominos in the example but tetrominos in the puzzle?
I'd like to know how to become a paid-up UKPA member too. Last time I asked I was told I had a free year for helping out at the 2014 WSC/WPC but that will have expired now.
The solution is only unique if you assume that there are no puppies which are not small, are not brown and do not have long hair.
Does the Screen Test mean that we need to bring a laptop?


Once again the Opening night movie at the Milwaukee Film Festival was a documentary. This year that documentary was Stumped. The film is a continuation of the short film of the same name that played a few years ago at the Milwaukee Film Festival. I love that the festival organizers like to take chance with opening up with a documentary and this one while it might not be a great film it was a crowd pleaser.
Last year at the Milwaukee Film Festival one of my favorite Milwaukee Short Films was The Fox in the Fan directed by Carol Brandt. This year she returns to the Festival with the world premiere of her first feature film Dear Coward on the Moon. Don't be deceived by the title, this is not a science fiction film, but a family drama mixed with fantasy. The film is a quiet observation of a family just trying to keep it together. The film is beautifully shot and has a great cast. It will definitely be one of the highlights of this year Milwaukee Film Festival.
One of the highlights for me at the Milwaukee Film Festival is the Milwaukee Show. The Milwaukee Show highlights great short films from local talent. Recently they added two shows so now we get even more great films to watch. This year the talent did not disappoint. Below are my 10 favorite films from the Milwaukee Shows.
Short films have the ability to tell a compelling story in a short amount of time. They can be funny, sad, serious, or scary. There are no limits on what a short film can be except short. I saw over 50 short films at the Milwaukee Film Festival and listed here are my Top 5 Short Fiction movies and my Top 5 Short Documentaries.
Every year the Milwaukee Film Festival brings hundreds of films to Milwaukee for 2 weeks. When they release the films that will be playing it's always a guessing game to figure out what films to see since most of the movies are ones I never heard of. This year I set a new record for number of movies I saw unfortunately few failed to really impress me. Now there are a number of reasons why this could have happened. Either I did a really bad job at picking movies this year, or the films Milwaukee Film picked weren't very good. Odds are I just didn't pick very well. But there are a number of films that I did enjoy and I want to highlight them.
I am going to break up my list to my 5 favorite fiction films and 5 favorite documentaries. I am going to start with just my favorite features but check back for my favorite shorts and my 10 Favorite Milwaukee Shorts.
Lots to delve into so let's get started.
When I tell people I am going to the Milwaukee Film Festival one of the first things they ask is "do they show anything good?" Of course they do. With over 300 films playing there is something for everyone; it's all a matter of finding ones you will like. What people might not realize is just because the Milwaukee Film Festival doesn't have the name recognition like Sundance or Toronto it doesn't mean its sub-par festival.
The festival guide makes it easy for you to find movies you might like. They have their Quick Picks based on what kind of movies you like and who you are going with. If you never been to a film fest before this is a great place to start. Last year instead of writing up a list of movie recommendations or what movies I plan on going to see (my tastes aren't for everyone) what I did was highlight things that make the Milwaukee Film Festival special. Not only are there great movies but it's an excellent opportunity to experience different things. No matter what movies you like there are things at the festival everyone should take advantage of. And this list is only the film related things. There are plenty of other great events surrounding the festival like live music, special gatherings, panels, and parties.


The First Yoga Studio to. . .
In 2008, Lake Tahoe Yoga opened as Svadhyaya Yoga (have fun pronouncing that one). Svadhyaya (svah-dee-yah-yah) means Self study and this is the focus of everything that happens at Lake Tahoe Yoga. Studio owner Jenay is consistently learning, growing and creating . . .and failing.
In 2008, there was only one other studio in Tahoe South located out in the Tahoe Keys. There was no place to practice Yoga in the Stateline area. When she opened Svadhyaya Yoga, it was the first studio available for Nevada-side practitioners to join in and learn the practice.
In 2009, Jenay brought the practice outdoors, combining two of her favorite things: Yoga and the beach! Svadhyaya Yoga Studio became the first Yoga Studio in Tahoe South to offer both studio and beach classes.
From late May/Early June through October, you can join Beach Asana classes that are held both in the mornings and evenings. The instructors, trained by Jenay are skilled at varying the practices and know all the tricks for making movement on the beach accessible or challenging.
You can find our practice spot by turning right at the end of the Nevada Beach driveway and heading to the North End of the beach. Then, keep your eyes open for our rainbow-colored flags.
In 2010, one of the practitioners at LTY brought a news article into the studio about Paddle Yoga in San Diego. This sparked an idea and Jenay did the footwork to find a location with which LTY could collaborate and offer the practice.
A little experimentation, a lot of practice, and years of devotion & consistency has resulted in the best Paddle Yoga classes on Lake Tahoe. South Tahoe Stand Up Paddle is the best connection LTY could ever have. Not only is it easy to access the water from their boathouse, they store, maintain and provide boards for use. In addition, we get to use Riviera Paddle Boards every season. The lack of boat traffic results in crystal clear, calm waters that create incredible images in the photos that are taken during every single class.
You can't be everything for everyone. Jenay is a Rajahatha Yoga Teacher which means that every class includes a focus upon traditional Yoga philosophy and practices. She does her best to adapt these practices to our modern times and make them accessible for all.
Her team includes instructors whom she has trained and continues to guide and support as they learn to meld the practices that they enjoy with their training in Rajahatha. LTY offers a variety of practices that vary from gentle to active. It is important to read the class descriptions or speak with one of the instructors prior to attending.
No two classes are ever the same as our teachers are adept at varying the sequencing and the practice in order to make sure everyone joining gets what they need. Raja is the practice of internal awareness and mindfulness while Hatha is the practice of effort. Every class includes both.
We believe that we are the Best Yoga Studio because we are the best at doing what we do. Jenay and the team at LTY will continue to learn, to grow, to create. . .and to fail. While we do so, we hope that you will join us for the practice.


Ladies come enjoy an evening of fashion fun. You can add to your closet by using Diva Dollars to bid on a host of fashion items.
Your $10 admission gets you $500 Diva Dollars to spend. BUT if $500 is not enough, additional Diva Dollars packages will be available for purchase.


I started out enthusiastically, but then other things overtook me.
Well I am going to have another go at starting this blog.
you won't read it unless I write it.
So let's see how we go.
Due to an overwhelming amount of comment spam, I have changed the restrictions on commenting.
If you do want to comment you will find you now have to log in via Typekey.
for any blog powered by Moveable Type.
After just deleting nearly 1000 trackbacks, I have also disabled this feature.
I will try to change this in the future, but for the moment, this is the way it will have to be.
As with many of us, when we started blogging we spent lots of time setting up our blogs. Now the reality of the amount of time maintenance takes has set in. I don't spend nearly as much time as I would like blogging, I don't want to be spending large amounts of the time I do have on maintenance.
11am & 3pm – 6pm.
I wonder if you are carrying a wounded soul?
morning. In the course of his research, Mitroff interviewed a number of CEOs.
fifties, in good physical shape, and happily married with three "great kids."
it didn't take long in the interview for a deep wound in his soul to surface.
agent of evil, Needless to say, this does not sit well with my self-concept."
What do we do with such dilemmas?
because they are lazy and they don't have any commitment to the corporation.
On the other hand we know how this came to be — see Agency Theory and Shareholder Value.
term to long term value. A small step. A step nevertheless.
religion we have priests, rabbis, mullahs and teachers. We also have heretics.
In personal health we have doctors and medical practitioners of all varieties.
Szasz). Somewhere in that mix, and across all fields of endeavour we have 'gurus'.
conversation. In short, they felt we were out to 'screw them'.
alter. In the book were all the possible scenarios that could face a business.
they hoped they were paying for.
the hard work of being a leader.
we were delighted to make the acquaintence of Colin and Patrina.
Just semantics perhaps, but for some reason Spiral Path felt there was a difference.
was determined by something outside of us.
Hmmm. We wonder what you think?
We've just been reading World Vision Australia CEO, Tim Costello's chapter in the recent Australian Institute of Management publication, Love @ Work.
say we've read most of the books he refers to.
slavery in all British colonies. [and that] Wilberforce died three days later.
Tim uses culture change "guru"
physical and emotional health but of their souls as well.
tribal wisdom and New Age views on particle physics and human nature.
dilemma is not to think about spirituality so much as think about Love.
the common good and not their self-interest alone.
We hope you buy the book.


text:
Logo Series
State Series
Archery Series
Elk Series
Fish Series
Truck Series
Turkey Series
Bird Series
Whitetail Deer Series
T-shirt Collaboration Series
Hank Shaw
National Wildlife Federation
Non-Lead Partnership
Pheasant Forever
Quail Forever
Randy Newberg
Remi Warren
Seek Outside
Sportsmen for the Boundary Waters
The Hunting Dog Podcast
Theodore Roosevelt Conservation Partnership
Wild Sheep Foundation
Hunt Camp
Arkansas Snow Goose
Conservation Contributors
Home / Stories /
Strange Times - A Sportsman's Thoughts on COVID-19
by Josh Mills, Hunt to Eat Ambassador
We are in some strange times, aren't we?
The prospect of severe alteration of the daily schedule had me staring at the familiar Costco sign and wondering if I had the gumption to go in and brave the crowds that most certainly were inside. Everyone's been subject to the stories seen on social media. Hysteria over toilet paper. People grappling over everyday goods like pasta, chicken and again, toilet paper.
Seriously, why the fixation on TP? I don't get it.
I was really there to stock up on items I knew I would likely need. You know, the essentials…Bourbon, beer, and a couple of bottles of wine. School was canceled for 6 weeks and the parents of Washington were being forced into a new career of home school parents. Courage we all need.
With that I found myself walking the store just observing, and eventually in the meat aisle. In front of the rotisserie chickens, a good 20 people anxiously waited for dinner to be pulled off the rack and put in their cart when it hit me hard…
Thank god I'm a hunter and an angler.
The line between dependent and independent was laid bare. Back at home, I am fortunate to have a modest lineup of fish, fowl, and beast sitting in my freezer, a bank of security in the midst of what I am starting to feel is a generational event that we've never experienced in my life. The anxiety that I felt around the store that day was palpable.
I take great joy in the experience that is time afield and in the river where a lot of the time the goal is centered in the harvest. When the dogs work the field, we take great joy when a rooster hits the ground and is added to the game bag. We marvel at the accomplishment of a successful shot on a bull elk after months of preparation and how about the high fives exchanged when a salmon hits the net and goes into the cooler?? We collectively spend way more than the worth of the meat in the act of hunting and fishing…but knowing when the chips are down the notion that you can bring home the bacon when needed is a thing of beauty.
Maybe some of that excitement is in knowing that you're depositing checks into your family's food bank of security? Knowing that we're going to eat, regardless of a food delivery schedule to a supermarket is a calming feeling.
There's no judgment on the other shoppers that I watched in Costco that day. We're living in a scary moment in history. To say that I could unplug my family from the industrial food chain that we live in right now is false, but at least fractionally there's less dependence on it when it comes to protein for our families.
We won't be fighting over the last steak in the grocery aisle…I can promise you that.
So what's next? How to proceed?
I'd say there's a hell of a lot of opportunity in being a resource to the greater community as a whole.
First, let's be honest. There are a lot of super-successful hunters and anglers out there with more in their freezer than they can ever eat in a year. To borrow a Rinella line, this is the best time ever to practice venison diplomacy and offer up the bounty to those in need. It could be the hard-up family down the street, a senior that can't get out to shop for themselves or a hundred other people in your life that could possibly use the gift of game. You can spare that package of burger, smoked trout or pheasant. You really can.
Second, take the opportunity to engage interested parties in hunting and fishing. So many people are likely open to the food side of hunting and taking a modest piece of control of their food supply back. There's a great deal of money being spent on the R3 initiatives (Recruitment, Retention and Reactivation) and this may be the grandest opportunity to get people excited about the outdoors, hunting and fishing we've ever seen. Ever.
The Covid-19 outbreak is a trying time for everyone involved. There won't be an aspect of society that won't be affected. It's a generational event that will cause shifts in our society for decades, possibly generations to come. Some bad, but the glass half full perspective that I have to adhere to tells me that a lot of proactive and positive changes will be brought about. Let's examine again how we get our food, and in turn remind each other that while hunting and fishing are sports, they're really about food and security.


text:
What is the difference between Black and Green tea?
Although the colour and flavour of tea is very different, black, green and Chinese tea are indeed made from the same type of tea plant (Camellia sinensis), which is native to East and South Asia.
The main difference between Japanese green tea and other teas is that green tea leaves are steamed after the harvest. The steaming process stops the oxidation process and maintains the natural green colour, fragrance and important nutrition. It is one of the less processed types of tea.
Different types of Green tea
Gyokuro is one of the world's most premium teas. Only 0.3% of tea produced in Japan is Gyokuro.
The tea plants are shaded for 3 weeks prior to harvesting, which reduces astringency and enhances flavor. This procedure gives the tea its smooth, full-bodied flavour and mellow sweetness.
Due to its rareness, Gyokuro usually costs 2-3 times more than Sencha.
Sencha : Most Popular Japanese green tea. It is produced all over Japan and 70% of Japanese tea production is Sencha.
The higher the grade, the more delicious the tea with the fragrance of soft leaves.
Grown in full sunlight, its refreshing flavour and the right balance of bitterness & sweetness is perfect as an everyday tea.
Fukamushi means deeply steamed. The leaves are steamed about twice longer than regular Sencha.
Due to the longer exposure to the steam's heat, they become powdery and provide stronger aroma with darker green colour.
Matcha is finely powdered tea made from Tencha, which like Gyokuro is grown in the shade and then processed.
It is used for traditional tea ceremony and a wide range of Japanese confection.
Matcha is like a finely ground form of Gyokuro - the plantation is covered to avoid sunshine about 20 days before picking. Unlike Gyokuro, there is no rolling process after steaming. The leaves are dried and stone-ground just before shipping.
Since it is in a powder form, it can readily used in cooking and baking.
Genmai-cha: Green tea combined with roasted brown rice, some grains of which have popped. It has a distinctive savoury aroma and flavour.
Matcha Genmai Cha
Matcha Genmai-cha is Genmai-cha mixed with Matcha powder.
Matcha Genmai cha has a similar flavour to plain Genmaicha but offers richer taste because of added Matcha power. Nutty and fresh. The colour is more green than light yellow.
Harvest seasons and grades
First harvest (Shin-cha, Ichiban-cha) : Harvested between late April and early May, shin-cha offers the best quality and aroma in Sencha kind. Tea bush saves nutrients in winter and release them in spring when new shoots start growing.
Second harvest tea (ni-bancha): After 2 weeks of first harvest, new shoots start growing and they will be ready for the second harvest in about 45 days (likewise for the 3rd harvest). Second harvest tea grows quickly in full sun. Compared to Shin-cha, second harvest is less rich in flavor and less expensive.
Bancha: Late harvest (3rd harvest and after) is called Bancha. Bancha tea leaves are harder and stems are also used to make this tea.
For Tea Lovers
Recipes & Tea info


text:
Farmingville, NY – On January 24, Supervisor Ed Romaine (right) and Councilwoman Michael Loguercio (left) were in Bellport for the demolition of an abandoned home located at 82 Beaver Dam Road. It was the Town's first demolition of 2017. The house sustained fire damage nearly 10 years ago and has been vacant and boarded ever since. The structure has deteriorated over the years and become a source of numerous resident complaints. It was demolished by the Town in accordance with Chapter 73 of the Town Code which provides a "fast track" to rid neighborhoods of unsafe structures. The cost of demolition and debris removal is the responsibility of the property owner, and the Town places a lien on the property that is then placed on the tax bill. The County reimburses the Town and then they collect the money from the property owner.
Supervisor Romaine said, "In 2016, we demolished 52 "zombie houses" and I expect to meet and exceed that number this year. Houses like this impact negatively on the quality of life and property values in the community, but thanks to work by our Law Department we are cleaning up neighborhoods across Brookhaven Town."
Councilman Loguercio said, "This house was not only an eyesore, it was an attractive nuisance that posed a danger to the residents nearby, especially children. I join the Supervisor in his commitment to rid Brookhaven Town of abandoned and derelict houses and I will continue to target those in my district that need to come down."
⇐Previous Town Demolishes Burned Out Zombie House in ShirleyNext⇒ Supervisor Romaine Celebrates Fourth of July at Patchogue Village Parade


#TravelPH - #TreeTopPH - Tree Top Adventure Baguio: Experience the extreme!
You might also want to try another branch of Tree Top Adventure Subic located at the JEST Area, Upper Mau Cubi Point Subic Bay Freeport Zone. For more information, you could contact (074) 442-0800 or 0932 404 1112. You could also visit our website www.treetopadventureph.com. To be more updated, you could like our Facebook page www.facebook.com/treetopadventurecamp and follow us on Instagram @tree_top_adventure.


The Range interface represents a fragment of a document that can contain nodes and parts of text nodes.
A range can be created using the createRange() method of the Document object. Range objects can also be retrieved by using the getRangeAt() method of the Selection object or the caretRangeFromPoint() method of the Document object.
There also is the Range() constructor available.
There are no inherited properties.
Returns a Boolean indicating whether the range's start and end points are at the same position.
Returns the deepest Node that contains the startContainer and endContainer nodes.
Returns the Node within which the Range ends.
Returns a number representing where in the endContainer the Range ends.
Returns the Node within which the Range starts.
Returns a number representing where in the startContainer the Range starts.
Returns a Range object with the global Document as its start and end.
There are no inherited methods.
Sets the start position of a Range.
Sets the end position of a Range.
Sets the start position of a Range relative to another Node.
Sets the end position of a Range relative to another Node.
Sets the Range to contain the Node and its contents.
Sets the Range to contain the contents of a Node.
Collapses the Range to one of its boundary points.
Returns a DocumentFragment copying the nodes of a Range.
Removes the contents of a Range from the Document.
Moves contents of a Range from the document tree into a DocumentFragment.
Insert a Node at the start of a Range.
Moves content of a Range into a new Node.
Compares the boundary points of the Range with another Range.
Returns a Range object with boundary points identical to the cloned Range.
Releases the Range from use to improve performance.
Returns the text of the Range.
Returns a constant representing whether the Node is before, after, inside, or surrounding the range.
Returns -1, 0, or 1 indicating whether the point occurs before, inside, or after the Range.
Returns a DocumentFragment created from a given string of code.
Returns a DOMRect object which bounds the entire contents of the Range; this would be the union of all the rectangles returned by range.getClientRects().
Returns a list of DOMRect objects that aggregates the results of Element.getClientRects() for all the elements in the Range.
Returns a boolean indicating whether the given node intersects the Range.
Returns a boolean indicating whether the given point is in the Range.
The definition of 'Range' in that specification. Living Standard Do not use RangeException anymore, use DOMException instead.
Made the second parameter of collapse() optional.
Added the methods isPointInRange(), comparePoint(), and intersectsNode().
The definition of 'Extensions to Range' in that specification. Working Draft Added the method createContextualFragment().
The definition of 'Extensions to Range' in that specification. Working Draft Added the methods getClientRects() and getBoundingClientRect().
The definition of 'Range' in that specification. Obsolete Initial specification.
Notes Starting with Firefox 13, the Range object throws a DOMException as defined in DOM 4, instead of a RangeException defined in prior specifications.
Chrome Full support Yes Edge Full support Yes Firefox Full support 24 IE No support No Opera Full support 15 Safari Full support Yes WebView Android Full support Yes Chrome Android Full support Yes Edge Mobile Full support Yes Firefox Android Full support 24 Opera Android Full support 15 Safari iOS Full support Yes Samsung Internet Android ?
Chrome Full support Yes Edge Full support 12 Firefox Full support Yes IE Full support 11 Opera Full support 15 Safari Full support 9 WebView Android Full support Yes Chrome Android Full support Yes Edge Mobile ? Firefox Android Full support Yes Opera Android Full support 15 Safari iOS ? Samsung Internet Android ?
Notes Since April 2014 this method is a no-op in Chrome.
Notes Starting in Firefox 15.0, this method is a no-op and has no effect.
Notes Since August 2015 this method is a no-op in WebKit-based browsers.
Chrome Full support Yes Edge Full support 12 Firefox Full support 4 IE Full support 9 Opera Full support 15 Safari ? WebView Android Full support Yes Chrome Android Full support Yes Edge Mobile Full support Yes Firefox Android Full support 4 Opera Android Full support 15 Safari iOS ? Samsung Internet Android ?
Chrome Full support Yes Edge Full support 12 Firefox Full support 4 IE Full support 9 Opera Full support 9 Safari Full support Yes WebView Android Full support Yes Chrome Android Full support Yes Edge Mobile Full support Yes Firefox Android Full support 4 Opera Android Full support 9 Safari iOS Full support Yes Samsung Internet Android ?
Chrome Full support Yes Edge Full support 17 Firefox Full support 17 IE No support No Opera Full support 15 Safari ? WebView Android Full support Yes Chrome Android Full support Yes Edge Mobile Full support Yes Firefox Android Full support 19 Opera Android Full support 15 Safari iOS ? Samsung Internet Android ?
Chrome Full support Yes Edge Full support 15 Firefox Full support Yes IE No support No Opera Full support 15 Safari ? WebView Android Full support Yes Chrome Android Full support Yes Edge Mobile Full support Yes Firefox Android Full support Yes Opera Android Full support 15 Safari iOS ? Samsung Internet Android ?
Chrome Full support Yes Edge Full support Yes Firefox Full support 4 IE Full support 9 Opera Full support 9 Safari Full support Yes WebView Android Full support Yes Chrome Android Full support Yes Edge Mobile Full support Yes Firefox Android Full support 4 Opera Android Full support Yes Safari iOS Full support Yes Samsung Internet Android ?


As usual there will take place the wonderful FAI di Primavera. The event is organized by Fondo Italiano per l'Ambiente (FAI – Italian Fund for Environment), a no-profit organization preserving and promoting Italian cultural heritage, and will open to public almost 600 Italian hidden treasures. Guided tours will be in Italian and for free donation.


text:
\section{Introduction}

Magnetic fields comparable to that of our Sun appear in the internal regions of all cool, low-mass solar-type stars, in small or higher scales \citep{lammer15}. The presence of the magnetic field can affect the evolutionary stages of a star and is responsible for its magnetic activity.
The evidence of the magnetic field presence is the emergence of dark spots in active regions on the stellar surface. The number of spots appearing and disappearing in the stellar disk varies in cycles. This behaviour observed in the Sun shows an 11 year-cycle, but it also happens in other stars.

The HK-project using the Mount Wilson Observatory, investigated hundred of stars by observing the Ca II HK lines to find stellar cycles similar to the solar case, with 52 of them showing this periodic behaviour \citep{bau95}. Using the Mount Wilson data, \cite{saar99} also studied stellar cycles and multiple cycles. From these observations, they estabilished the relation between stellar rotation period, $P_{\rm rot}$, and magnetic cycle period, $P_{\rm cycle}$ as a function of the Rossby number, dividing the stars into active (A) and inactive (I) branches, which were distinguished by the number of rotations per cycle and activity level. Later, several long photometric records for a significant sample of stars became available, and other studies of the stellar cycles were performed \citep{olah09, mg02, lovis11}.

Along with the 11 year cycle of the Sun, there are other short-durations cycles, known as quasi-biennial oscilations (QBO). \cite{fletch10} found a quasi-biennial period of 2 years in the low-degree solar oscillation frequencies of the Sun after separating this signal from the influence of the dominant 11 year solar cycle. In addition, \cite{bazil14} reported  solar QBOs with the time scale of 0.6$-$4 years. In other stars, some short period variations were also reported. The first were detected by \cite{bau95} in two stars from the Mount Wilson survey, HD 76151 with 2.52 years and HD 190406 with 2.60 years. \cite{olah09} found fifteen stars showing multiple cycles by the analysis of Ca II emission. Using high cadence SMARTS HK data, \cite{meta10} discovered a 1.6 year magnetic activity cycle for the solar twin $\iota$ Horologii and found two cycles in $\epsilon$ Eridani, one of 2.95 years and a long-term cycle of 12.7 years. \cite{ege15} also found a short-period $\sim$ 1.7 year for the solar analogue HD 30495. Using Kepler observations,  \cite{salabert16} discovered from the analysis of frequency shifts a 1.5 year variation for the solar analog KIC 10644253, that could be a short-period or quasi-biennal oscillation.

Other techniques such as monitoring starspots can provide information on stellar cycles. Evidence of the spots can be found by analysing planetary transits in the star lightcurve \citep{nutz11,sanchis11,soap13}. Small variations in the lightcurve occur because when the planet eclipses the star it may occult spots on the stellar surface, causing an increase in the luminosity during the transits. \cite{sil03} developed  a method to infer the properties of starspots from high precision transit photometry, such as size, position and intensity. Here we use this model to characterize the magnetic cycle of two active solar-type stars: Kepler-17 and Kepler-63. To cross check this model, we adopted a new technique, called here as transit residuals excess, to verify the variation of the level of activity in both stars.

This paper is organized as follows. Section \ref{sec:observations} provides an overview of the observations for Kepler-17 and Kepler-63. Section \ref{sec:spotmodel} explains the first method adopted in this work, whereas the next section describes the physical parameters of the modelled spots. Section \ref{sec:starmag} presents the second method and the results for the activity cycles obtained with both methods. The paper finishes with the discussions and conclusions, presented in Sections \ref{sec:disc} and \ref{sec:conclu}, respectively.

\section{Observations}
\label{sec:observations}

The stars analysed in the present work, Kepler-17 and Kepler-63, were observed by the Kepler satellite. This mission was responsible for collecting data of thousand of stars and planets (\cite{boru10}). The duration of the mission was scheduled for 3.5 years, initially planned to finish in 2012 but was extended to 2016 (K2 mission) (see \cite{howell14}). The telescope has an aperture of 95 cm and explores about $1.6 \times 10^{5}$ stars in a field of 150deg$^{2}$. It was projected to discover Earth size planets located in the habitable zone of stars (dwarfs F to K). To keep the solar panel towards the Sun, the spacecraft needed to rotate about its axis by 90$\,^{\circ}$ every 93 days, this time interval is known as ``quarter''. A total of 2,327 planets were confirmed until now and there are 4706 planet candidates \footnote{http://kepler.nasa.gov/, July 2017}.

The lightcurves can be obtained from the MAST \footnote{http://archive.stci.edu/} (\textit{Mikulski Archive for Space Telescopes}) database. The observation of the target stars are made along sixteen quarters and consists of long (one data point each 29.4 minutes) and short cadence data ($\sim$ 1 min time resolution). For our study, we selected only short cadence lightcurves, because we are interested in short time scale variations, with planetary transits over the whole period of operation of the satellite.

The stars analysed here are active solar type stars. Kepler-17 is a G2V star with age $<$ 1.8 Gyr and Kepler-63 is also a young G-type star (subclass still unknown) of about 200 Myr. Both stars are accompanied by a giant planet in close orbit (Hot Jupiter): Kepler-17b has $\approx 2.5$ Jupiter masses and an orbital period of 1.486 day (\cite{desert11}), while Kepler-63b has $\approx$ 0.4 Jupiter masses and an orbital period of 9.434 days. During the 1240 days of observation of the Kepler mission, a total 834 possible transits were detected for Kepler-17, while Kepler-63 was observed for 1400 days and 150 transits were registered. The lightcurve of these stars shows that they are very active and marked by rotational modulations caused by the presence of starspots, with a peak-to-peak variation of $6\%$ for Kepler-63 and $4\%$ for Kepler-17. The active regions of Kepler-17 was previously analysed by \cite{bonomo12}, who found spots area of 10 to 15 times larger than the solar ones and evidences of a differential rotation in latitudes similar to the those presented in the Sun. Study of spot evolution in this star was also perfomed by \cite{davenport15}. The physical properties of the stars and their planets are shown in Table \ref{table:tab1} and Table \ref{table:tab2}, respectively.

\begin{table*}[!ht]
\refstepcounter{table}\label{table:tab1}
\resizebox{0.8\textwidth}{!}{\begin{minipage}{\textwidth}
\centering
\begin{threeparttable}
\begin{tabular}{cccccccc}
\multicolumn{8}{c}{\textbf{Table 1}}                                                                                \\
\multicolumn{8}{c}{Observational parameters of the stars}                                                                                \\
\toprule
\toprule
           & KIC Number & Mass {[}$M_{\odot}${]}   & Radius {[}R$_{\odot}${]}   & Age {[}Gyr{]}    & Effective temperature {[}K{]} & Rotation period {[}d{]} & Reference \\
Kepler-17 & 10619192   & 1.16 $\pm$ 0.06          & 1.05 $\pm$ 0.03            & $<$ 1.78 Gyr     & 5780 $\pm$ 80                 & 11.89 $\pm$ 0.15        & 1,2       \\
Kepler-63 & 11554435   & 0.984$^{+0.04}_{-0.035}$ & 0.901$^{+ 0.022}_{-0.027}$ & 0.2 Gyr & 5580 $\pm$ 50                 & 5.401 $\pm$ 0.014       & 3        \\
\bottomrule
\end{tabular}
\begin{tablenotes}
\item \textbf{References.} (1) \cite{bon12}, (2) \cite{desert11} and (3) \cite{sanchis13}.
\end{tablenotes}
\end{threeparttable}
\end{minipage}}
\end{table*}

\begin{table*}[!ht]
\refstepcounter{table}\label{table:tab2}
\resizebox{0.7\textwidth}{!}{\begin{minipage}{\textwidth}
\centering
\begin{threeparttable}
\begin{tabular}{llllllllll}
\multicolumn{10}{c}{\textbf{Table 2}}                                                                                \\
\multicolumn{10}{c}{Observational parameters of the planets}                                                                                \\
\toprule
\toprule
          & KIC Number                     & Mass {[}$M_{\rm jup}${]}                 & Radius {[}$R_{\rm jup}${]}               & Radius {[}$R_{\rm star}${]}          & Orbital                   & Inclination, $i$ {[}deg{]}                    & Semi-major                       & Semi-major                      & Reference \\
          &                                &                                      &                                      &                                  & Period {[}d{]}            &                                               & axis, $a$ {[}AU{]}               & axis, $a$ {[}$R_{\rm star}${]}      &           \\
Kepler-17b & \multicolumn{1}{c}{10619192 b} & \multicolumn{1}{c}{2.45 $\pm$ 0.014} & \multicolumn{1}{c}{1.442$^{a}$}      & \multicolumn{1}{c}{0.138$^{a}$}  & \multicolumn{1}{c}{1.485} & \multicolumn{1}{c}{87.2 $\pm$ 0.15}           & \multicolumn{1}{c}{0.0279$^{a}$} & \multicolumn{1}{c}{5.729$^{a}$} & 1,2       \\
Kepler-63b & \multicolumn{1}{c}{11554435 b} & \multicolumn{1}{c}{$<$ 0.3775}       & \multicolumn{1}{c}{0.593$^{a}$} & \multicolumn{1}{c}{0.0662$^{a}$} & \multicolumn{1}{c}{9.434} & \multicolumn{1}{c}{87.8 $^{+0.018}_{-0.019}$} & \multicolumn{1}{c}{0.081$^{a}$}  & \multicolumn{1}{c}{19.35$^{a}$} & 3     \\
\bottomrule
\end{tabular}
\begin{tablenotes}
\item $^{a}$ Modified values to obtain a better fit of each transit lightcurve.
\item \textbf{References.} (1) \cite{bon12}, (2) \cite{desert11} and (3) \cite{sanchis13}.
\end{tablenotes}
\end{threeparttable}
\end{minipage}}
\end{table*}

\section{Spot modelling}
\label{sec:spotmodel}

To characterize the spots, we adopted the transit model proposed by \cite{sil03} that uses small transit photometry variations to infer the properties of starspots. The passage of the planet in front of the star may occult solar-like spots on the stellar surface, producing a slight increase in the luminosity detected during a short period (minutes) of the transit. This occurs because the spot is darker (cooler region) than the stellar photosphere and causes a smaller decrease in the intensity than when it blocks a region without spots. This effect is shown in Figure ~\ref{fig:figura1_1}.

This model simulates a star with quadratic limb darkening as a 2D image and the planet is assumed to be a dark disk with radius $R_{p}/R_{\rm star}$, where $R_p$ is the radius of the planet and $R_{\rm star}$ is the radius of the primary star. For each time interval, the position of the planet in its orbit is calculated according to its parameters: inclination angle $i$ and semi-major axis $a$. The simulated lightcurve results from the intensity integration of all the pixels in the image for each planet position during the transit. All the simulations are performed considering a circular orbit, that is null eccentricity. Applications of such model are described in \cite{sil03} for HD 209458, \cite{sil10} and \cite{sil11} for the active star CoRoT-2.

An example of the application of this model is shown in Fig. \ref{fig:figura1_2} for the 120th transit of Kepler-17, where the top panel shows the fit with three spots (red curve), together with the model of a star without any spots (yellow curve). The bottom panel of Fig. \ref{fig:figura1_2}, shows the residuals from the subtraction of the spotless model, where the spots became more evident, as the three ``bumps'' seen in the residuals. An estimation of the noise presented in the Kepler data is given by the CDPP (Combined Differential Photometric Precision, see \cite{christiansen12}), computed for each quarter in the lightcurve. We considered the uncertainty in the data, $\sigma$, as being the average of the CDPP values in all quarters. Only the ``bumps'' that exceed the detection limit of 10$\sigma$ are assumed as spots and modelled. The modelled spots are constrained within longitude of $\pm$ 70$\,^{\circ}$ (dashed lines) to avoid any distortions caused by the ingress and egress branches of the transit. In this region the lightcurve measurements are much less accurate than in the central part of the transit due to the steep gradients in intensity. The maximum number of spots modelled per transit was set to 4, with an exception for only one transit of Kepler-17, where it was necessary to fit 5 spots.

\begin{figure}[ht]
  \centering
\includegraphics[scale=0.40]{spots_model_final.pdf}
  \caption[Model]{\textit{Top}: 2D Simulated image of a star with quadratic limb darkening and one spot, and its planet, assumed as a dark disk. \textit{Bottom}: Resulting light curve from the transit, with the ``bump'' due to spot-crossing by the planet.}
\label{fig:figura1_1}
\end{figure}

The model assumes that the spots are circular and described by 3 parameters: size (in units of planetary radius $R_p$), intensity with respect to the surface of the star (in units the maximum intensity at disc centre, $I_c$), and  longitude (allowed range is $\pm$70$^{\circ}$ to avoid distortions of the ingress and egress of the transit). For Kepler-17, where the orbital plane is aligned with the stellar equator, the latitude of the spots remains fixed and equal to the planetary transit projection onto the surface of the star. This latitude is -14$\,^{\circ}$.6 and corresponds to an inclination angle of 87.84$\,^{\circ}$, that was arbitrary chosen to be South. Moreover, the foreshortening effect is taken into account for the spots near the limb. Due to the high obliquity of the orbit of Kepler-63b, the planet occults several latitudes of the star from its equator all the way to the poles.

\begin{figure*}[ht]
  \centering
\includegraphics[scale=0.70]{method1.pdf}
  \caption[Model]{The 120th transit from Kepler-17 illustrates a typical example of the spot fit by the model developed by \cite{sil03}. \textit{Top}: Transit lightcurve with the model of a spotless star overplotted (yellow). \textit{Bottom}: Residuals of the transit lightcurve after subtraction of a spotless star model. The red curve shows the fit to the data ``bumps'' on both panels.}
\label{fig:figura1_2}
\end{figure*}

It was necessary to refine the values from the semi-major axis and planet radius taken from the literature \citep{desert11} for Kepler-17b and \citep{sanchis13} for Kepler-63b, to obtain a better fit for each transit lightcurve. Therefore, we used 5.729 $R_{\rm star}$ (Kepler-17b) and 19.35 $R_{\rm star}$ (Kepler-63b) for the semi-major axis, while for the planet radius we adopted 0.0662 $R_{\rm star}$ and 0.138 $R_{\rm star}$, respectively (see Valio et al. 2016 (to be submitted) and Netto and Valio, 2016 (submitted). These values represent 8$\%$ and 6$\%$ (radius) and 4$\%$ and 1$\%$ (semi-major axis) increase, respectively for Kepler-17 and Kepler-63, with respect to the initial values given in \citep{bon12} and \cite{sanchis13}.

The residuals from each transit lightcurve were fit using this model. We performed initial guesses manually, for the longitude of the spot, $lg_{spot}$, obtained from the approximate central time of the ``bump'', $t_{s}$ (in hours), computed as follows:

\begin{equation}
t_{s} = \left\lbrace 90\,^{\circ} - \arccos \left[ \frac{\sin(lg_{s})) \cos(lat_{s})}{a} \right] \right\rbrace \frac{P_{\rm orb}}{360 ^{\circ}} 24 \rm h
\end{equation}

\begin{figure}[!ht]
  \centering
\includegraphics[scale=0.18]{hist_int_k17.pdf}
\includegraphics[scale=0.18]{hist_radius_k17.pdf}
\includegraphics[scale=0.18]{hist_temperature_k17.pdf}
\includegraphics[scale=0.18]{hist_lg_k17.pdf}
  \caption[Hist]{Histograms of the spots parameters for Kepler-17: spots intensity (in units of $I_c$) (\textit{top}), spots radius (in units of $R_{p}$) (\textit{middle}), and temperature (\textit{bottom}). }
\label{fig:figura1_3}
\end{figure}

\begin{figure}[!ht]
  \centering
\includegraphics[scale=0.18]{hist_int_k63.pdf}
\includegraphics[scale=0.18]{hist_radius_k63.pdf}
\includegraphics[scale=0.18]{hist_temp_k63.pdf}
\includegraphics[scale=0.18]{hist_lg_k63.pdf}
  \caption[Hist]{Same as Fig. \ref{fig:figura1_3} for Kepler-63.}
\label{fig:figura1_4}
\end{figure}

\noindent where $P_{\rm orb}$ is the orbital period, $lat_{s}$ is the latitude of the spot in the stellar surface and $a$ is the semi major axis. The number of spots were determined a priori for each transit. For the radius and intensity, we considered initial guesses of 0.5 $R_{p}$ and 0.5 $I_{c}$. The parameters for the spots are chosen from the best fit obtained by the minimization of the $\chi^2$, calculated using the AMOEBA routine \citep{press92}.

\section{Spots physical parameters}
\label{sec:spotpar}

Using the model transit lightcurve proposed by \cite{sil03} and described in the previous section, we analysed each transit separately and the small variations in the luminosity detected during the transit were interpreted as the presence of a spot occulted by the planet. A total of 507 transits for Kepler-17 and 122 for Kepler-63 showed ``bumps'' in the lightcurve residuals above the adopted threshold of 10 CDPP.
From the analysis of these ``bumps'', we obtained a total of 1069 spots (Kepler-17) and 297 (Kepler-63) and estimated their average parameters (radius, intensity and longitude). Furthermore, from the relative spot intensity it is possible to estimate its temperature by considering that both the photosphere and the spots radiate like a blackbody, according to the equation:

\begin{equation}
\frac{I_{\rm spot}}{I_{\rm star}}=\frac{e^{h \nu / K_{B}T_{\rm eff}}-1}{e^{h \nu / K_{B}T_{0}}-1}
\end{equation}

\noindent from which we obtain the temperature of the spots:

\begin{equation}
T_{0}= \frac{K_{b}}{h \nu\ \ln \left( f_{i} \left( e^{h \nu/K T_{\rm eff}} -1 \right) +1 \right) }
\end{equation}

\noindent where $K_{b}$ and $h$ are the Boltzmann and Planck constants, respectively, and $\nu$ is the frequency associated with a wavelength of 600 $nm$, $f_{i}$ is the fraction of spot intensity with respect to the central stellar intensity $I_{c}$ obtained from the fit, and $T_{eff}$ is the effective temperature of the star. Considering an effective temperature of 5781 $K$ for Kepler-17 and 5576 $K$ for Kepler-63, we found an average spot temperature of 5000 $\pm$ 600 $K$ and 4800 $\pm$ 400 $K$, respectively, for both stars.

These results are summarized in Table \ref{table:tab3}. The distributions of the parameters are presented in Figure~\ref{fig:figura1_3} and Figure~\ref{fig:figura1_4}. In the case of Kepler-63, we can observe that the radii of the spots are between the range 0.3 up to 2.0 $R_p$. For the intensity, we have a variation from 0.1 to 0.8 $I_c$. The temperature varies from 3000K to 5400K. The longitude varies from -50 to +50$^{\circ}$. For the other star, Kepler-17, the variation of the spots parameters are the following: 0.1 to 2.0 $R_p$ for the radius, 0.1 to 1.0 $I_c$ for intensity, 2000K to 6000K for the temperature, and $\pm$50$^{\circ}$ is the range for the longitude. Note that in Kepler-17 the longitude of the spots are concentrated preferentially in the center of the transit, and for this reason, there is a decrease when the values approach $\pm$70$^{\circ}$, however the same does not happen for Kepler-63, due to the fact that the orbit of the planet crosses several latitudes. For further details of the spot modelling, see Valio et al. (2016) (to be submitted) and Netto $\&$ Valio (2016) (submitted) for Kepler-63.

\begin{table}[!ht]
\centering
\refstepcounter{table}\label{table:tab3}
\begin{tabular}{lcc}
\multicolumn{3}{c}{\textbf{Table 3}}                               \\
\multicolumn{3}{c}{Average values for the parameters of the spots} \\
\midrule
\midrule
                   & Kepler-17                  & Kepler-63               \\
Radius [$R_p$]     & 0.6 $\pm$ 0.3              & 0.8 $\pm$ 0.3   \\
Radius [km]        & (57 $\pm$ 28) $\times 10^{3}$ & (33 $\pm$ 12) $\times 10^{3}$     \\
Intensity [$I_c$]  & 0.54 $\pm$ 0.19            & 0.47 $\pm$ 0.16   \\
Temperature [K]    & 5000 $\pm$ 600             & 4800 $\pm$ 400        \\
Longitude [$^{\circ}$] & -3 $\pm$ 30               & -7 $\pm$ 30 \\
\bottomrule
\end{tabular}
\end{table}

\section{Stellar magnetic activity}
\label{sec:starmag}

Our aim is to characterize the magnetic cycles of Kepler-17 and Kepler-63. For this purpose we adopted two different methods as proxies for the stellar activity: (1) number and flux deficit of the spots modelled in the previous section and (2) estimate of the excess residuals during transits. These procedures were applied to a total of 583 transits for Kepler-17 and 131 transits for Kepler-63. Details and results from both methods are described below.

\subsection{Spot modelling}
\label{ssec:spotmodel2}

In the case of the Sun, the number of spots on the solar surface is the most common proxy of its activity cycle and displays a periodic variation every 11 years or so. Similarly, the number of spots that appears at the surface of a star varies in accordance with the stellar magnetic cycle. Thus by monitoring the number of spots, during the approximate 4 years of observation of the Kepler stars, it is in principle possible to detect stellar cycles.

\begin{figure}[!ht]
  \centering
\hspace*{-1cm}
\includegraphics[scale=0.25]{k17_NS_e.pdf}
\hspace*{-1cm}
\includegraphics[scale=0.25]{k17_FLUX_e.pdf}
  \caption[Number]{Number of spots (\textit{Top}) and total flux deficit (\textit{bottom}) caused by the spots in Kepler-17 derived from the transits analysed with the method described in Sections~\ref{sec:spotmodel} and \ref{sec:spotpar}.}
\label{fig:figura1_5}
\end{figure}

\begin{figure}[!ht]
  \centering
\hspace*{-1cm}
\includegraphics[scale=0.25]{k63_NS_e.pdf}
\hspace*{-1cm}
\includegraphics[scale=0.25]{k63_FLUX_e.pdf}
  \caption[Flux]{Number of spots ({Top}) and total flux deficit (\textit{bottom}) in Kepler-63.}
\label{fig:figura1_6}
\end{figure}

Another way to estimate stellar activity is calculating the flux deficit resulting from the presence of spots on the star surface. The spots contrast is taken to be $1-f_{i}$, where $f_{i}$ is the relative intensity of the spot with respect to the disk center intensity $I_{c}$. A value of $f_{i}$ = 1 means that there is no spot at all. The relative flux deficit of a single spot is the product of the spot contrast and its area, thus for each transit the total flux deficit associated with spots was calculated by summing all individuals spots:

\begin{equation}
F \approx \sum (1-f_{i})(R_{\rm spot})^{2}
\end{equation}

To the resulting flux deficit and spot number we apply a running mean over a range of five data points. Note that due to this process, the number of spots may have non-integer values. Also, to remove possible aperiodic or long duration trends in these time series, we applied a quadratic polynomial fit to the data and then subtracted it. Due to this procedure, the number of spots and the flux deficit can be negative. Figures \ref{fig:figura1_5} and \ref{fig:figura1_6} show these treated results for the number of spots (top, in blue) obtained from modelling each transit and the total flux deficit (bottom, in green) for both stars.

\begin{figure*}[!ht]
  \centering
\includegraphics[scale=0.45]{k17_NS_FLUX_lomb_freqsig_e.pdf}
  \caption[Lomb]{(\textit{Top}) Power spectrum indicating the periodicity of the spots number (blue) and of the flux deficit (green) for Kepler-17. The highest peak is indicated by the vertical dashed lines and is 410 $\pm$ 60 days for the spot number and 410 $\pm$ 50 days for the spot flux. (\textit{Bottom}) P-values associated to each frequency from the periodogram, the significance level is assumed to be 3$\sigma$.}
\label{fig:figura1_7}
\end{figure*}

\begin{figure*}[!ht]
  \centering
\includegraphics[scale=0.45]{k63_NS_FLUX_lomb_freqsig_e.pdf}
  \caption[Lomb]{Power spectrum indicating the periodicity of the spots number (\textit{top}) and of the flux deficit (\textit{bottom}) for Kepler-63. The highest peak is indicated by the dashed lines and is 460 $\pm$ 60 days for the spot number and 460 $\pm$ 50 days for the spot flux.}
\label{fig:figura1_8}
\end{figure*}

\begin{figure*}[!ht]
  \centering
\includegraphics[scale=0.40]{k17_NS_FLUX_FOLDED_e.pdf}
  \caption[Folded]{Three folded data of Kepler-17 for both spot number and total flux deficit, the 410 days periodicity clearly showing.}
\label{fig:figura1_9}
\end{figure*}

\begin{figure*}[!ht]
  \centering
\includegraphics[scale=0.40]{k63_NS_FLUX_FOLDED_e.pdf}
  \caption[Folded]{Same as Fig.\ref{fig:figura1_9} for Kepler-63, indicating the periodicity of 460 days of the spot data.}
\label{fig:figura1_10}
\end{figure*}

\begin{figure*}[!ht]
  \centering
\hspace*{-7mm}
\includegraphics[scale=0.39]{method2.pdf}
  \caption[Subtracted transit]{\textit{Top}: 100th transit lightcurve of Kepler-17, overplotted is a simulated lightcurve without spots (solid curve). \textit{Bottom}: Residuals of the subtracted light curve. The dashed vertical lines correspond to longitudes $\pm$ 70$^{\circ}$.}
\label{fig:figura1_11}
\end{figure*}

\begin{figure}[!ht]
  \centering
\hspace*{-7mm}
\includegraphics[scale=0.24]{k17_ATIV_e.pdf}
\hspace*{-7mm}
\includegraphics[scale=0.24]{k63_ATIV_e.pdf}
  \caption[Activity]{Activity level from the integration of all lightcurve residuals excess during transits as described in Sect.~\ref{sec:Residuals} for Kepler-17 (\textit{top}) and Kepler-63 (\textit{bottom}).}
\label{fig:figura1_12}
\end{figure}

A Lomb Scargle periodogram (LS) \citep{scargle82} is perfomed on these time series  to obtain the period related to the magnetic cycle. In addition, we applied a significance test to quantify the significance of the peaks from the LS periodogram. For this, we assumed the null hypothesis as: (a) there is no periodicity in the data, and (b) the noise has a Gaussian distribution, thus the periodogram power spectrum in any frequency of the data will be exponentially distributed. The statistical significance associated to each frequency in the periodogram is determined by the p-value (\textrm{p}). The smaller the p-value, the larger the significance of the peak.  The corresponding values for p-value in critical values are given by $z = \sqrt(2) \rm erf^{-1} (1-2p)$. We adopted the significance level $\alpha$ as being 3$\sigma$ (\textrm{p} $\pm$ 0.0013). If the p-value is less or equal to the significance level, our null hypothesis is rejected, otherwise, it is not rejected. The result of the significance test is plotted below the periodogram for each star, in Figures~\ref{fig:figura1_7} and ~\ref{fig:figura1_8}. The uncertainty of the peaks in the periodogram is given by FWHM of the peak power.

By computing the Lomb-Scargle periodogram, it is possible to detect the existence of a periodicity in the spot number and flux deficit throughout the 4 years of observation. This result is presented on Figures \ref{fig:figura1_7} and \ref{fig:figura1_8}. In both situations, a long term periodicity is found. For Kepler-17, a prominent peak is seen at 410 $\pm$ 60 days (number of spots) and 410 $\pm$ 50 days (flux deficit). There is also another significant periodicity in $\sim$ 104 days ($f$ = 0.0096 days$^{-1}$) appearing in both cases. This peak might be a harmonic, because it is approximately four times the value of the frequency from the main peak ($f$ = 0.0024 days$^{-1}$, P = 410 days). However, as we are interested only in long term periodicities, we adopted $P_{\rm cycle}$ = 410 days as being the most relevant peak for our case. This yields a magnetic cycle of approximately 1.12 yr.

Kepler-63 shows a periodicity of 460 $\pm$ 60 days taking into account the total number of spots, and 460 $\pm$ 50 days for the flux deficit, as shown in Fig.~\ref{fig:figura1_8}. This corresponds to a cycle of about 1.27 $\pm$ 0.20 yr. There is also a strong peak at $\sim$ 111 days for the total flux deficit, however this period appears at the number of spots periodogram with a very small significance, thus we do not consider this peak.

We folded the data of both spot number and total flux deficit by the dominant period obtained in the periodograms. These results are presented in Figures \ref{fig:figura1_9} (Kepler-17) and \ref{fig:figura1_10} (Kepler-63), and in both cases we obtained three periods during the time of observation of the stars (1240 days for Kepler-17 and 1400 days for Kepler-63).

\subsection{Transit residuals}\label{sec:Residuals}

The second method adopted in this work consists in subtracting from the transit lightcurves a modelled lightcurve of a star without spots. The result from this subtraction is the residual. An example of this method is shown in Figure~\ref{fig:figura1_11} for the 100th transit of Kepler-17. An excess during the transit is clearly seen and is due to the presence of spots occulted by the planet. Next we integrated all residuals excess within $\pm$ 70$^{\circ}$ longitude of the star (delimited by the dashed lines of Fig.~\ref{fig:figura1_11}) thus obtaining another proxy for the stellar activity. This residual excess resulting from all transits is plotted in Fig.~\ref{fig:figura1_12}, and is seen to oscillate during the period of observation.

\begin{figure*}[!ht]
  \centering
\includegraphics[scale=0.40]{k17_ATIV_lomb_freqsig_e.pdf}
\includegraphics[scale=0.40]{k63_ATIV_lomb_freqsig_e.pdf}
  \caption[Lomb]{Lomb Scargle periodogram applied to the integrated transit residuals excess of Kepler-17 (\textit{top}) and Kepler-63 (\textit{bottom}). The highest peak, indicated by a dashed line, corresponds to a periodicity of 494 $\pm$ 100 days for Kepler-17 and 465 $\pm$ 40 days for Kepler-63.}
\label{fig:figura1_13}
\end{figure*}

A quadratic polynomial fit was also applied to this time series and subtracted, removing any possible trends. Its Lomb Scargle periodogram is shown in Fig.~\ref{fig:figura1_13}, where a noticeable peak is seen at 490 $\pm$ 100 days (1.35 $\pm$ 0.27 yr) for Kepler-17 and 460 $\pm$ 40 days (1.27 $\pm$ 0.12 yr) for Kepler-63. These periodicities show a p-value below the 3$\sigma$ significance level, confirming their significance. The value obtained for Kepler-63 is similar to that from the first approach, and corresponds to a 1.27 year-cycle. There is also a notable peak at $\sim$ 205 days ($f$ = 0.00485 days$^{-1}$), but this peak does not appear in the first approach (neither for spot number or flux deficit), thus we do not consider it. The three folded data with the obtained periodicity is shown in Figure \ref{fig:figura1_14} for Kepler-17 and Kepler-63. On the other hand, the cycle period estimate for Kepler-17 agree within the uncertainty, as shown in Figure \ref{fig:figura1_15}. All the results for the magnetic cycle obtained with the two methods are listed in Table \ref{table:tab4}.

\begin{figure*}[!ht]
  \centering
\includegraphics[scale=0.40]{k17_ATIV_FOLDED_e.pdf}
\includegraphics[scale=0.40]{k63_ATIV_FOLDED_e.pdf}
  \caption[Folded]{Activity level data folded three times with the resulting periodicity. \textit{Top}: Kepler-17 (490 days) and \textit{bottom}: Kepler-63 (460 days).}
\label{fig:figura1_14}
\end{figure*}

\begin{figure*}[!ht]
  \centering
\includegraphics[scale=0.35]{k17_significance_e.pdf}
  \caption[Significance]{Comparison between the peak significance obtained from the first method for the flux deficit (green) and the second method (purple). The frequency peak obtained in the second method falls inside the uncertainty from the first approach.}
\label{fig:figura1_15}
\end{figure*}

\begin{table*}[!ht]
\refstepcounter{table}\label{table:tab4}
\resizebox{1.0\textwidth}{!}{\begin{minipage}{\textwidth}
\centering
\begin{tabular}{lccc}
\multicolumn{4}{c}{\textbf{Table 4}}                                      \\
\multicolumn{4}{c}{Magnetic activity cycle periods}                       \\
\toprule
\toprule
          & \multicolumn{2}{c}{Spot Modelling} & Transit residuals excess \\
          & (Number of spots)   & (Spot Flux)  &                          \\
\midrule
Kepler-17 & 1.12 $\pm$ 0.13 yr    & 1.12 $\pm$ 0.16 yr      & 1.35 $\pm$ 0.27 yr                  \\
Kepler-63 & 1.27 $\pm$ 0.16 yr  & 1.27 $\pm$ 0.14 yr                 & 1.27 $\pm$ 0.12 yr                  \\
\bottomrule
\end{tabular}
\end{minipage}}
\end{table*}

\section{Discussion}
\label{sec:disc}

We have estimated the period of the magnetic cycle, $P_{\rm cycle}$, for two active solar-type stars, Kepler-17 and Kepler-63, by applying two new methods: spot modelling and transit residuals excess. The results obtained from both methods are presented in Table \ref{table:tab4}. For Kepler-63, we found the same result in the different approaches. The other star, Kepler-17, however, has a $P_{\rm cycle}$ obtained with the second method that is within the uncertainty range from the first approach. Considering that, we confirm that the results in both methods agree with each other and assure the robustness of the methods.
Next, we compare our results to those stars, with their magnetic cycle, $P_{\rm cycle}$, reported in the literature. The observational data from \cite{saar99} and \cite{lor05} are the records of the CaII H$\&$K emission fluxes of the stars observed at the Mount Wilson Observatory and also analysed by \cite{bau95}. \cite{olah09} studied multi-decadal variability in a sample of active stars with photometric and spectroscopic data observed during several decades. \cite{mg02} performed long-term photometric monitoring of solar analogues. \cite{lovis11} took a sample of solar-type stars observed by the HARPS\footnote{High Accuracy Radial velocity Planet Searcher} spectrograph and used the magnitude and timescale of the Ca II H$\&$K variability to identify activity cycles.

\begin{figure*}[!ht]
  \centering
\includegraphics[scale=0.35]{plot_cyclev2.pdf}
  \caption[Cycle]{Activity cycle periods, $P_{\rm cycle}$, versus stellar rotation period, $P_{\rm rot}$, for a sample of stars cited in the literature. The dashed vertical lines connect different periods found for the same stars, i.e: stars exhibiting two cycles.}
\label{fig:figura1_16}
\end{figure*}

Two distinct branches were reported for the cycling stars \citep{saar99, bohm07}: the active (blue line) and inactive (green line), classified according to their activity level and number of rotations per cycle (plotted in Fig. \ref{fig:figura1_16}). The majority of  the stars analysed by \cite{lovis11} falls in the inactive branch, the Sun, however, with its 11 year-cycle appears in between the two branches. In Figure \ref{fig:figura1_16} we observe the relation between $P_{\rm cycle}$ (stellar cycle period) and $P_{\rm rot}$ (stellar rotation period) for all selected samples, first studied by \cite{bau96}. The vertical dashed line joins data for the same star (stars with multiple periodicities detected). Kepler-63 (blue star in  Fig. \ref{fig:figura1_16}) is an active star and in the rotational period-cycle relation follows the trend set by stars in the active branch. On the other hand, Kepler-17 (blue star) lies close to the inactive stars branch, but shows a cycle period quite close to the short-period cycle obtained by \cite{ege15} for the active star HD 30495, of $P_{\rm cycle} \sim$ 1.7 year, $P_{\rm rot}$ = 11 days, and the one analysed by \cite{salabert16} for the young solar analog KIC 10644253 ($P_{\rm cycle}$ $\sim$ 1.5 year, $P_{\rm rot}$ = 10.91 days).

\section{Conclusions}
\label{sec:conclu}

In the present work we applied two new methods to investigate the existence of a magnetic cycle: spot modelling and transit residuals excess. Two active solar-type stars were analysed, Kepler-17 ($P_{\rm rot}$ = 11.89 days and age $<$ 1.8 Gyr) and Kepler-63 ($P_{\rm rot}$ = 5.40 days and age = 0.2 Gyr). With the first method, we obtained $P_{\rm cycle}$ = 1.12 $\pm$ 0.16 yr (Kepler-17) and $P_{\rm cycle}$ = 1.27 $\pm$ 0.16 yr (Kepler-63), and for the second approach: $P_{\rm cycle}$ = 1.35 $\pm$ 0.27 yr (Kepler-17) and $P_{\rm cycle}$ = 1.27 $\pm$ 0.12 yr (Kepler-63). The results from both methods agrees with each other, considering that the value found for Kepler-17 in the second approach falls within the uncertainty of the first method. Kepler-17 and the solar analogue HD 30495 found by \cite{ege15} have a rotation period of approximately 11 days, and both show a short-cycle, which is $\sim$ 1.7 yr for HD 30495. However, this star also shows a long cycle of $\sim$ 12 years, that agrees well with the active branch. As observed previously by \cite{bohm07}, some stars that are located in the active branch, could also show short cycles falling in the inactive branch. This might be the case of Kepler-17, that is also an active star, showing a spots area coverage of 6$\%$, much higher than the Sun, where it is less than 1$\%$, and may also have a long cycle periodicity. Unfortunately, as we are constrained by the period of observation ($\leq$ 4 years) of the Kepler telescope, it is not possible to investigate if Kepler-17 has a longer cycle. On the other hand, $P_{\rm cycle}$ of the young star Kepler-63, fits well within the active stars branch. Morever, \cite{meta10} found a 1.6 year magnetic cycle for the exoplanet host star $\iota$ Horologii observed during 2008 and 2009, that seems to be in between Kepler-17 and Kepler-63 in the cycle-rotation relation.

The intensity of a magnetic field is controlled by the dynamo process, and associated with  differential rotation. Our analysis to identify activity cycle periods is essential for a deep investigation about how stellar dynamos work. \cite{bohm07} and \cite{durn81} suggest that the two branches of stars in the $P_{\rm rot}-P_{\rm cycle}$ diagram are possibly ruled by different kinds of dynamo, exhibiting different ratios for $P_{\rm cycle}/P_{\rm rot}$. In addition, B\"ohm-Vitense brings up that the active branch can be driven by a dynamo operating in the near-surface shear layer, while in the inactive stars branch, the shear layer of the dynamo is located at the base of the convection zone. This combination between the analysis of the time variation in the stellar activity and the stellar rotation periods can also be crucial to determine the differential rotation rates of the star, which is fundamental to generate the magnetic field in the stellar interiors. All these indicate that activity cycles play a key role in understanding the evolution of stars.

\acknowledgments

This work has been supported by grant from the Brazilian agency FAPESP ($\#$2013/10559-5). Raissa Estrela acknowledges a CAPES fellowship.

redpajama_set_name: RedPajamaArXiv


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