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Funding Circle powers past £50m as demand for non bank funding grows
By Bridging Loan Directory - 29th October 2012
Funding Circle, the online marketplace where people lend money directly to businesses, has passed the £50 million mark in new lending.
The business, which celebrated is second birthday recently, has lent more than £12 million since the beginning of August. Funding Circle is seeing growing support from small businesses keen to access finance at a time when banks are reluctant or unwilling to lend.
According to Laura McMullen, Business Development Director at Funding Circle, the significant jump in lending in the past two months demonstrates the importance of alternative funding to provide support to businesses at a time when traditional banking sources seem to be unable to respond positively.
She said, "The primacy of banks as the default funding source for small businesses is waning. We are seeing more professional advisers coming to us as they become aware of new sources of finance that are more responsive to their clients' needs. It comes as no surprise that Funding Circle's simple, flexible facility is providing a significant fresh resource for business owners and their advisers."

redpajama_set_name: RedPajamaCommonCrawl


text:
Perspectives: RAL and the uncertain future of snow sports
27 Oct 2022 By Contributor
Ruapehu Alpine Lifts' uncertain future underscores the volatility of commercial ski businesses and snow sports as climate change uncovers the slippery slope of unsustainability, writes University of Waikato's Holly Thorpe.
Research shows the ways we currently conduct snow sports are unsustainable, says Thorpe.
With New Zealand's two major North Island ski fields in financial trouble, the combined impact of Covid-19 on national and international tourism and this year's very poor snow season has hit hard. But this may be only a sign of things to come as climate change affects snow sports globally.
Ruapehu Alpine Lifts (RAL), which runs the Turoa and Whakapapa ski fields, has debts of NZ$40 million and has gone into voluntary administration. Despite calls for government support, Minister of Tourism and Economic and Regional Development Stuart Nash has said there will be no more funding beyond the $15 million in loans already provided since 2018.
For now, then, the future of snow sports on the slopes of Mt Ruapehu remains uncertain, directly and indirectly affecting many businesses and livelihoods. But RAL is not the first ski company to struggle under increasingly unpredictable winters.
Shorter or less predictable ski seasons and warmer temperatures are already causing closures elsewhere. Some foreign ski fields are pivoting to cater for summer recreational tourism such as mountain biking and hiking.
Some ski resorts in North America, Europe and Australia are now facing uncertain futures. One US study found revenues could fall 40-60% (on average) by 2080. The research is clearly showing the ways we currently practise and consume snow sports are unsustainable.
No business like snow business
Scientists from the National Institute of Water and Atmospheric Research (NIWA) recently modelled the potential impact of climate change on snow levels in New Zealand. Their report showed an average gradual decrease in snow at nearly all elevations as the century progresses.
While all ski areas will experience this, the effects will vary depending on their location and elevation. Under the warmer climate change predictions, the study showed snow depths between 83% and 45% of current maximums at lower elevation sites by 2040.
By 2090, this will be further reduced (on average) to approximately 48% to 9% of current maximum snow depths. According to NIWA snow and ice scientist Dr Jordy Hendrikz:
From these results we expect to see a gradual change in snow levels but […] we should be able to continue to make snow, even under a more extreme climate scenario, right out to the 2090s.
The report was considered good news for New Zealand snow areas, which are reportedly "confident they will adapt to any risks from climate change". But is a future for ski fields based mostly on making artificial snow really good news?
While some may see innovations in snow-making technologies as future-proofing the ski industry, resorts becoming highly dependent on their capacity to make artificial snow raises serious ethical and environmental concerns. The process uses huge amounts of water and chemical and biological additives, with ramifications for mountain ecosystems and potentially human health.
Greening the snow?
This presents a dilemma. For those privileged enough to visit often expensive ski resorts, the pristine mountain environment is central to the experience. Yet ski resorts are far from environmentally friendly.
With thousands of visitors every day, they have enormous carbon footprints when various factors are accounted for: travel to and from ski fields (planes, 4WD vehicles, buses), the energy demands of lifts and facilities, snow grooming and machinery maintenance.
It's true that over the past decade there have been attempts to green the snow industry. Ski resorts have invested in sustainability planning and adaption strategies, from recycling food waste to using wind turbines and solar energy. Some clothing and equipment companies are also working to produce more sustainable and eco-friendly products.
Despite signs of change, however, there are questions about whether a form of greenwashing is taking place in the snow sports industry, as it has across the sports sector in general, where many organisations have made superficial claims of environmentalism. Research has shown ski resorts can vary widely in their communication of sustainability efforts versus their actual levels of environmentally responsible action.
Snow businesses produce enormous carbon footprints when factoring in travel, energy demands from lifts and facilities, snow grooming, and machine maintenance. Image: Zack Keay
From pleasure to politics
Research also suggests that committed lifestyle sports participants like skiers, snowboarders and surfers can develop close relationships with the natural environment that encourage more environmentally sustainable practices.
For example, Protect Our Winters (POW) is an international non-profit organisation (with a New Zealand chapter) where skiers, snowboarders, hikers, climbers and mountain bikers work with scientists, policymakers and politicians to advocate for greater protection of mountains.
As some scholars have observed, however, there is a degree of ecological irony in an industry and its participants claiming to be environmentally conscious while maintaining highly mobile and consumerist lifestyles.
There are other strands of resistance, too. In Aotearoa New Zealand and around the world, mountain ownership and management have long been integral to Indigenous struggles for self-determination. Local communities have recently challenged expansion plans by ski resorts for both cultural and environmental reasons.
Many ski resorts have been built on stolen land. They still represent the privilege and wealth of settler societies. Only a few acknowledge the historical and contemporary politics of ski resort land use.
Any efforts to develop a sustainable ski industry, then, will have to include conserving the environmental integrity and cultural diversity associated with the mountains themselves. But the fact remains that climate change means the future is bleak for the snow sports industry.
While the full effects will be felt by some regions, resorts and communities more than others, the policy questions raised by the troubles at RAL and Ruapehu's iconic ski fields are urgent: what is the future of snow sports, and what are the ethics of pursuing such activities in a climate emergency?
Holly Thorpe is a professor in Sociology of Sport and Gender at the University of Waikato.
8 Dec 2022 Ruapehu mayor welcomes ski fields support
7 Dec 2022 Govt throws $6m lifeline to RAL ski fields
6 Dec 2022 Community group touts crowdfunding up to $30m to save Mt Ruapehu skifields
24 Nov 2022 RAL life pass holders launch petition
22 Nov 2022 150 trade creditors owed nearly $1m by RAL
21 Nov 2022 RAL life pass holders scoped for $2.5k fee plus annual $250 levy
1 Nov 2022 RAL secures $4m emergency loan from MBIE, ANZ
21 Oct 2022 Ruapehu Alpine Lifts owes $44.3m – report


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Lately there has been a lot of talk about fake OPI polishes being sold, not only online, but also in stores. While there is the occasional fake floating out there, I do think that most of this is blown out of proportion. So I have decided to write a little guide to help you identify your OPI bottle.
For the first nine years after OPI launched in 1989, the bottle design stayed the same. After that there were numerous little changes made almost every year. Size and shape of the bottle varies slightly, as well as print size.
The first bottle design was relatively simple. It would list the three major cities, plus the measurement units using uppercase characters. On bottles made before the mid 90s, the print is located slightly lower on the bottle.
This is the transition year where they slightly started the bottle change process. The old bottle style remains, but the labeling is slightly different. They also added the e symbol, which indicates that the packaging and content adheres to European average standards, in other words, to indicate that there is indeed 15 ml in the bottle. The measurement units are now all lowercase characters.
The new bottle design is introduced. Instead of listing the three major cities, it now lists the French and Spanish translations of 'Nail Lacquer'.
The German translation of 'Nail Lacquer' is added to the design.
The measurement units are switched around, ml is now listed first.
The measurement units now use uppercase characters again.
On the back a warning message and the address are printed, all in uppercase. No warning symbols are printed.
The European distributor is now listed on the back, underlined and all uppercase. Two warning symbols are printed. The US address is printed in uppercase, except for 'Hollywood'. Also printed is 'MADE IN USA'.
The zip code is now listed for the European distributor, and the address is no longer underlined. A third warning symbol is added at the end of 2002.
A fourth warning symbol is added, indicating the shelf life in months. Initially it would say 36 months, but by late 2006 it was changed to 24 months (this is because of the 2006 formula change, more about this below).
The bottle labels seem to have changed even more through the years, so I'll write a little bit about that as well. With a few exceptions, all labels are two-layer labels. The top layer can be peeled off, and the ingredients are listed on the backside of the top layer.
back then were shorter, and started with OPI instead of NL. The address is printed around the edge, along with the phone number (note the parenthesis around the area code).
My bottles do not have the top label anymore, any help with this is greatly appreciated!
The top layer lists the bar code on the top half. The name is printed in the middle, with the production code stamped below. On the bottom half it says PEEL HERE, with the color code in between the two.
The second layer lists the name and code in the middle, and around the edges the address and phone number. Note that the phone number has changed, as well as the formatting.
The production code is now listed above the name. The color code is now printed directly below the name. The bottom layer remains the same.
The name is now printed along the top edge of the label, with the color code below. The production code is printed in the middle, above the bar code. The bottom layer remains the same.
the US. In Europe OPI polishes have been truly B3F since the end of 2006 due to the strong enforcement of the ban by the European union.
This collection has a label identical to the green label mentioned above, except it is brown colored. The color codes start with NN instead of NL. These polishes are B3F.
There are two sets of designer series polishes available. The older ones are not B3F and contain toluene. The top layer label lists the color code first, then the production code. The name is printed in the middle, with Designer Series printed in red. The newer Designer Series polishes have a label that is identical to the regular green label, except it is all printed in a dark red. These are B3F.
These are one-layer labels, since US law does not require the listing of ingredients on salon products. The print is black and resembles the bottom layer of the green labels. Since the ingredients are not listed, they MAY contain toluene – although this is very unlikely for newer polishes.
Promo bottles are marked not for resale. These are not very common.
Not much is known about this collection, only the shades that were part of it, and the color codes. The bottle labels are all one layer only, list the production code, as well as two of the warning symbols.
When I got Rainforest, I sent an e-mail to OPI asking if it was the real thing, and what collection it is from. They told me it was released in 2005 as part of the Color Centric collection. The thing that confuses me about this, is that the bottles are obviously older than 2005, and nothing pops up when I Google that collection name. My bottle of Creme de Menthe has the late 90s design, and my bottle of Rainforest has the 2001 design.
Since 2001, OPI engraved all bottles with a 8-digit production code along the upper side of the bottle. There are several different fonts used for this, and not consistently. Sometimes small and narrow, sometimes bigger and rounder. In some rare cases, it is engraved in the cap instead of the bottle.
Since 2008, OPI also stamped a production code along the bottom side of the bottle, matching the code stamped on the bottom label. This stamp can be easily removed by scratching with a fingernail, or using some acetone. So keep in mind that when you got the bottle from an unauthorized seller, it might not have the stamp on the side.
NOTE: The font used for the stamping is related to the font used for the engraving. If the engraving is bigger and rounder, so is the stamping.
In 2006, OPI introduced the Pro-Wide brush. This brush is wider and more rectangular shaped for better nail coverage. The stem is oval instead of round, and has the OPI logo etched near the top.
The color looks off and not familiar. Sometimes OPI bottles are refilled with random polishes and sold mostly on eBay.
Spelling or grammar mistakes in the print.
Bottles labeled just 'Pink' or '306'.
The information in this article is carefully compiled from examining my own collection of (hundreds of) OPI bottles, the information provided by the official OPI book 'I'm Not Really A Waitress' and information provided by OPI via e-mail.
Some bottles may still use the old front and back print, while they are released a year after discontinuation of that particular design. Therefore, dating a bottle purely by its design might not be fully accurate. I suggest dating by label AND bottle design for a more accurate result.


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text:
"""
Test data augmentation of the small slices data set

Created on Thu Dec 21 14:59:42 2017

@author: mbarbier
"""
from keras.preprocessing.image import ImageDataGenerator
#from keras import model
from data_small import loadData
from module_utilities import removeFolderContents
import numpy as np
import itertools

print('-'*30)
print('Loading train data...')
print('-'*30)
imgs_train, imgs_test, imgs_mask_train_all, imgs_mask_test_all, imgs_id_test, imgs_id_train = loadData( 0.8, 16 )
images = np.expand_dims( imgs_train, axis = 3 )
masks_all = imgs_mask_train_all

print('-'*30)
print('Fuse masks to single multi-label image')
print('-'*30)
regionList = [ "cb", "hp", "cx", "th", "mb", "bs" ]
regionIdList = range(1, len(regionList)+1)
masks = np.zeros( masks_all[regionList[0]].shape )
for index in range(len(regionList)):
    region = regionList[index]
    value = regionIdList[index]
    masks = masks + value * masks_all[region]
masks = np.expand_dims( masks, axis = 3 )

print('-'*30)
print('Fuse masks to single multi-label image')
print('-'*30)
# we create two instances with the same arguments
data_gen_args = dict(featurewise_center=True,
                     featurewise_std_normalization=True,
                     rotation_range=90.,
                     width_shift_range=0.1,
                     height_shift_range=0.1,
                     zoom_range=0.1)
image_datagen = ImageDataGenerator(**data_gen_args)
mask_datagen = ImageDataGenerator(**data_gen_args)

# Provide the same seed and keyword arguments to the fit and flow methods
seed = 1

# Compute the statistics for data augmentation purposes (centering, normalization)
image_datagen.fit(images, augment=True, seed=seed)
mask_datagen.fit(masks, augment=True, seed=seed)

# The folders to save the extra images and corresponding masks of the data augmentation
augm_masks_folder = '/home/mbarbier/Documents/prog/DeepSlice/python/keras_small/augm_masks'
augm_images_folder = '/home/mbarbier/Documents/prog/DeepSlice/python/keras_small/augm_images'
fake_y = np.zeros( images.shape[0] )
image_generator = image_datagen.flow(
    x = images,
    y = fake_y,
    save_to_dir = augm_images_folder,
    save_prefix = 'augm_image',
    save_format = 'png',
    seed=seed)
mask_generator = mask_datagen.flow(
    x = masks,
    y = fake_y,
    save_to_dir = augm_masks_folder,
    save_prefix = 'augm_mask',
    save_format = 'png',
    seed=seed)

# combine generators into one which yields image and masks
train_generator = zip(image_generator, mask_generator)

# here's a more "manual" example
# Empty the dirs
removeFolderContents(augm_images_folder)
removeFolderContents(augm_masks_folder)
epochs = 20
for e in range(epochs):
    print('Epoch', e)
    batches = 0
    for x_batch, y_batch in train_generator:
        print('batch ' + str(batches) + ' : do nothing, save something?')
        #model.fit(x_batch, y_batch)
        batches += 1
        if batches >= len(images) / 32:
            # we need to break the loop by hand because
            # the generator loops indefinitely
            break

##model.fit_generator(
##    train_generator,
##    steps_per_epoch=20,
##    epochs=20)

#layer_dict = dict([(layer.name, layer) for layer in model.layers])

redpajama_set_name: RedPajamaGithub


Blood. 2007 Oct 15;110(8):3015-27. Epub 2007 Jul 16.
Lesional gene expression profiling in cutaneous T-cell lymphoma reveals natural clusters associated with disease outcome.
Shin J1, Monti S, Aires DJ, Duvic M, Golub T, Jones DA, Kupper TS.
Cutaneous T-cell lymphoma (CTCL) is defined by infiltration of activated and malignant T cells in the skin. The clinical manifestations and prognosis in CTCL are highly variable. In this study, we hypothesized that gene expression analysis in lesional skin biopsies can improve understanding of the disease and its management. Based on 63 skin samples, we performed consensus clustering, revealing 3 patient clusters. Of these, 2 clusters tended to differentiate limited CTCL (stages IA and IB) from more extensive CTCL (stages IB and III). Stage IB patients appeared in both clusters, but those in the limited CTCL cluster were more responsive to treatment than those in the more extensive CTCL cluster. The third cluster was enriched in lymphocyte activation genes and was associated with a high proportion of tumor (stage IIB) lesions. Survival analysis revealed significant differences in event-free survival between clusters, with poorest survival seen in the activated lymphocyte cluster. Using supervised analysis, we further characterized genes significantly associated with lower-stage/treatment-responsive CTCL versus higher-stage/treatment-resistant CTCL. We conclude that transcriptional profiling of CTCL skin lesions reveals clinically relevant signatures, correlating with differences in survival and response to treatment. Additional prospective long-term studies to validate and refine these findings appear warranted.
Gene filtering. A total of 22 283 probe sets were filtered using a noise envelope to eliminate genes with little cross-chip variability. The noise envelope was estimated on 14 HeLa cell lines and 5 Strategene samples. Two filters were used, resulting in gene sets of 6997 (α = 0.999) and 4204 (α = 0.9999) probe sets. Unsupervised analyses were done using the 4204-gene filter. Supervised analyses were done using the 6997-gene filter.
Consensus clustering. Consensus clustering indicates that 3 clusters is the greatest number of stable clusters across clustering techniques. Consensus heat maps produced by HC and SOMs for cluster number k = 3 are shown. The consensus heat map is a visual representation of the consensus matrix, which is a matrix of sample pairs. Each matrix entry is the proportion of times the pair's samples are clustered together across resampling iterations. In the heat map, a value of 1 (corresponding to 2 samples that are always clustered together) is represented by the color red, and a value of 0 (corresponding to 2 samples that are never clustered together) is represented by the color white.
Consensus clustering overlap matrices for the 3-cluster model.(A) Sample overlap comparing sample assignment between HC and SOMs. Entries are the number of samples in overlapping clusters. (B) Marker overlap between HC and SOMs. Gene markers for k = 3 clusters using HC and SOMs were evaluated to assess the number of markers held in common between clustering techniques. Entries are presented as: residual [no. observed | no. expected], where residual = (observed −expected) / sqrt (expected).
Hierarchical clustering heat map. This heat map shows partitioning of 63 samples and the top 593 genes with P values less than or equal to .025 and fold change greater than or equal to 2. The chart shows the top 15 GO terms for each cluster, ranked by FDR. Each GO term is accompanied by the number of up-regulated genes/the total number of genes included in the test group. All included GO terms have P values less than or equal to .05 and FDR less than or equal to .05.
Cluster composition based on clinical stage. Entries are presented as: residual [no. observed | no. expected], where residual = (observed −expected) /sqrt (expected). Yellow indicates relative deficiency of cluster with respect to the clinical stage, and green indicates enrichment of cluster with respect to the clinical stage, comparing observed with expected composition. Sample phenotype correlation showed cluster 1 to be composed of a roughly equivalent proportion of clinical stages. However, this breakdown was statistically enriched with stage IIB, or tumor stage, disease and lacking in stage IB disease. Cluster 2 was enriched with patch/plaque stage disease, with only 2 samples categorized as stage IIB and III. Cluster 3 showed depletion in stage IA and IIB disease and enrichment in stage IB and III disease. These findings were statistically significant, with a P value of .004.
Event-free Kaplan-Meier curves. Survival was evaluated using Kaplan-Meier analysis. Events included disease progression, large-cell transformation, and death. There were 10 events, including 7 deaths, 1 large-cell transformation after biopsy, and 3 patients who progressed despite systemic treatments. The log-rank test was used to determine significance of differences between survival curves. Event-free survival is shown (A) by clinical stage (P < .001); (B) by hierarchical cluster, using a 3-cluster partition (P = .028); and (C) by hierarchical cluster, using a 2-cluster partition (P = .02).
Histologic and immunophenotypical correlation with cluster. Representative biopsies are shown. Left panels are the hematoxylin-eosin stain, and right panels are immunohistochemical stains using monoclonal antibody to CD3. (A) Cluster 2: stage IA, untreated erythematous plaque on the chest. (B) Cluster 3: top 2 panels depict a stage IB lesion, while the bottom panel shows a stage III lesion. All images were acquired on a Nikon Eclipse E600 microscope (Nikon, Melville, NY) with a 10×/0.30 objective using a SPOT digital camera and image acquisition software (Diagnostic Instruments, Sterling Heights, MI).
Heat map showing gene selection for stage IA/IB compared with stage IIB/III. Our analysis yielded gene sets of 480 genes with FDR less than or equal to 0.05, using the gene filter for 6997 genes, ranked by signal-to-noise ratio. The chart shows the top 20 GO terms for each stage, ranked by FDR. Each GO term is accompanied by the number of up-regulated genes/the total number of genes included in the test group. All included GO terms have cutoffs of .05 for both P value and FDR.
Comparison with published results. Tracey et al examined genes included on the CNIO Oncochip microarray platform, a subset of the genes included on the Affymetrix HG-U133 microarray platform. They identified 2 main subgroups of patients using hierarchical clustering. We compared this to our 3-cluster division determined through consensus clustering. Sample clustering in the space of genes identified by Tracey et al showed significant consistency with our results, despite only 21% overlap between genes used in clustering. We also examined a less optimized 2-cluster structure of our data for comparison, and found relatively good overlap with the 2-cluster structure of Tracey et al. (A) 3-cluster structure. 79% of samples overall were correctly classified. This result was significant (P < .001). (B) 2-cluster structure. 87% of samples overall were correctly classified using a 2-cluster structure. The result was again significant (P < .001). (C) Gene correlation. Genes were similarly classified for 71% of 130 common genes. Genes associated with more aggressive disease by Tracey et al were found to be associated with more advanced disease in our study as well. This finding was significant (P < .001).


text:
Coronal mass ejection
This video shows the particle flow around Earth as solar ejecta associated with a coronal mass ejection strike.
A coronal mass ejection (CME) is a significant release of plasma and accompanying magnetic field from the solar corona. They often follow solar flares and are normally present during a solar prominence eruption. The plasma is released into the solar wind, and can be observed in coronagraph imagery.[1][2][3]
Coronal mass ejections are often associated with other forms of solar activity, but a broadly accepted theoretical understanding of these relationships has not been established. CMEs most often originate from active regions on the Sun's surface, such as groupings of sunspots associated with frequent flares. Near solar maxima, the Sun produces about three CMEs every day, whereas near solar minima, there is about one CME every five days.[4]
The largest recorded geomagnetic perturbation, resulting presumably from a CME hitting the Earth's magnetosphere, was the solar storm of 1859 (the Carrington Event), which took down parts of the recently created US telegraph network, starting fires and shocking some telegraph operators.[11]
DescriptionEdit
Follow a CME as it passes Venus then Earth, and explore how the Sun drives Earth's winds and oceans.
Arcs rise above an active region on the surface of the Sun.
Coronal mass ejections release large quantities of matter and electromagnetic radiation into space above the Sun's surface, either near the corona (sometimes called a solar prominence), or farther into the planetary system, or beyond (interplanetary CME). The ejected material is a magnetized plasma consisting primarily of electrons and protons. While solar flares are very fast (being electromagnetic radiation), CMEs are relatively slow.[5]
Coronal mass ejections are associated with enormous changes and disturbances in the coronal magnetic field. They are usually observed with a white-light coronagraph.
CauseEdit
The phenomenon of magnetic reconnection is closely associated with CMEs and solar flares.[6][7] In magnetohydrodynamic theory, the sudden rearrangement of magnetic field lines when two oppositely directed magnetic fields are brought together is called "magnetic reconnection". Reconnection releases energy stored in the original stressed magnetic fields. These magnetic field lines can become twisted in a helical structure, with a 'right-hand twist' or a 'left hand twist'. As the Sun's magnetic field lines become more and more twisted, CMEs appear to be a 'valve' to release the magnetic energy being built up, as evidenced by the helical structure of CMEs, that would otherwise renew itself continuously each solar cycle and eventually rip the Sun apart.[8]
On the Sun, magnetic reconnection may happen on solar arcades—a series of closely occurring loops of magnetic lines of force. These lines of force quickly reconnect into a low arcade of loops, leaving a helix of magnetic field unconnected to the rest of the arcade. The sudden release of energy during this process causes the solar flare and ejects the CME. The helical magnetic field and the material that it contains may violently expand outwards forming a CME.[9] This also explains why CMEs and solar flares typically erupt from what are known as the active regions on the Sun where magnetic fields are much stronger on average.
Satellite photo of aurora borealis stretching across Quebec and Ontario in the early morning of 8 October 2012.
Impact on EarthEdit
When the ejection is directed towards Earth and reaches it as an interplanetary CME (ICME), the shock wave of traveling mass causes a geomagnetic storm that may disrupt Earth's magnetosphere, compressing it on the day side and extending the night-side magnetic tail. When the magnetosphere reconnects on the nightside, it releases power on the order of terawatt scale, which is directed back toward Earth's upper atmosphere.
Solar energetic particles can cause particularly strong aurorae in large regions around Earth's magnetic poles. These are also known as the Northern Lights (aurora borealis) in the northern hemisphere, and the Southern Lights (aurora australis) in the southern hemisphere. Coronal mass ejections, along with solar flares of other origin, can disrupt radio transmissions and cause damage to satellites and electrical transmission line facilities, resulting in potentially massive and long-lasting power outages.[10][11]
Energetic protons released by a CME can cause an increase in the number of free electrons in the ionosphere, especially in the high-latitude polar regions. The increase in free electrons can enhance radio wave absorption, especially within the D-region of the ionosphere, leading to Polar Cap Absorption (PCA) events.
Humans at high altitudes, as in airplanes or space stations, risk exposure to relatively intense solar particle events. The energy absorbed by astronauts is not reduced by a typical spacecraft shield design and, if any protection is provided, it would result from changes in the microscopic inhomogeneity of the energy absorption events.[citation needed]
Physical propertiesEdit
A video of the series of CMEs in August 2010.
This video features two model runs. One looks at a moderate coronal mass ejection (CME) from 2006. The second run examines the consequences of a large coronal mass ejection, such as the Carrington-class CME of 1859.
A typical coronal mass ejection may have any or all of three distinctive features: a cavity of low electron density, a dense core (the prominence, which appears on coronagraph images as a bright region embedded in this cavity), and a bright leading edge.
Most ejections originate from active regions on the Sun's surface, such as groupings of sunspots associated with frequent flares. These regions have closed magnetic field lines, in which the magnetic field strength is large enough to contain the plasma. These field lines must be broken or weakened for the ejection to escape from the Sun. However, CMEs may also be initiated in quiet surface regions, although in many cases the quiet region was recently active. During solar minimum, CMEs form primarily in the coronal streamer belt near the solar magnetic equator. During solar maximum, they originate from active regions whose latitudinal distribution is more homogeneous.
Coronal mass ejections reach velocities from 20 to 3,200 km/s (12 to 1,988 mi/s) with an average speed of 489 km/s (304 mi/s), based on SOHO/LASCO measurements between 1996 and 2003. These speeds correspond to transit times from the Sun out to the mean radius of Earth's orbit of about 13 hours to 86 days (extremes), with about 3.5 days as the average. The average mass ejected is 1.6×1012 kg (3.5×1012 lb). However, the estimated mass values for CMEs are only lower limits, because coronagraph measurements provide only two-dimensional data. The frequency of ejections depends on the phase of the solar cycle: from about one every fifth day near the solar minimum to 3.5 per day near the solar maximum.[12] These values are also lower limits because ejections propagating away from Earth (backside CMEs) usually cannot be detected by coronagraphs.
Current knowledge of coronal mass ejection kinematics indicates that the ejection starts with an initial pre-acceleration phase characterized by a slow rising motion, followed by a period of rapid acceleration away from the Sun until a near-constant velocity is reached. Some balloon CMEs, usually the slowest ones, lack this three-stage evolution, instead accelerating slowly and continuously throughout their flight. Even for CMEs with a well-defined acceleration stage, the pre-acceleration stage is often absent, or perhaps unobservable.
Association with other solar phenomenaEdit
Video of a solar filament being launched
Coronal mass ejections are often associated with other forms of solar activity, most notably:
Solar flares
Eruptive prominence and X-ray sigmoids[13]
Coronal dimming (long-term brightness decrease on the solar surface)
Moreton waves
Coronal waves (bright fronts propagating from the location of the eruption)
Post-eruptive arcades
The association of a CME with some of those phenomena is common but not fully understood. For example, CMEs and flares are normally closely related, but there was confusion about this point caused by the events originating beyond the limb. For such events no flare could be detected. Most weak flares do not have associated CMEs; most powerful ones do. Some CMEs occur without any flare-like manifestation, but these are the weaker and slower ones.[14] It is now thought that CMEs and associated flares are caused by a common event (the CME peak acceleration and the flare impulsive phase generally coincide). In general, all of these events (including the CME) are thought to be the result of a large-scale restructuring of the magnetic field; the presence or absence of a CME during one of these restructures would reflect the coronal environment of the process (i.e., can the eruption be confined by overlying magnetic structure, or will it simply break through and enter the solar wind).
Theoretical modelsEdit
It was first postulated that CMEs might be driven by the heat of an explosive flare. However, it soon became apparent that many CMEs were not associated with flares, and that even those that were often started before the flare. Because CMEs are initiated in the solar corona (which is dominated by magnetic energy), their energy source must be magnetic.
Because the energy of CMEs is so high, it is unlikely that their energy could be directly driven by emerging magnetic fields in the photosphere (although this is still a possibility). Therefore, most models of CMEs assume that the energy is stored up in the coronal magnetic field over a long period of time and then suddenly released by some instability or a loss of equilibrium in the field. There is still no consensus on which of these release mechanisms is correct, and observations are not currently able to constrain these models very well. These same considerations apply equally well to solar flares, but the observable signatures of these phenomena differ.[citation needed]
Interplanetary coronal mass ejectionsEdit
Illustration of a coronal mass ejection moving beyond the planets toward the heliopause
CMEs typically reach Earth one to five days after leaving the Sun. During their propagation, CMEs interact with the solar wind and the interplanetary magnetic field (IMF). As a consequence, slow CMEs are accelerated toward the speed of the solar wind and fast CMEs are decelerated toward the speed of the solar wind.[15] The strongest deceleration or acceleration occurs close to the Sun, but it can continue even beyond Earth orbit (1 AU), which was observed using measurements at Mars[16] and by the Ulysses spacecraft.[17] CMEs faster than about 500 km/s (310 mi/s) eventually drive a shock wave.[18] This happens when the speed of the CME in the frame of reference moving with the solar wind is faster than the local fast magnetosonic speed. Such shocks have been observed directly by coronagraphs[19] in the corona, and are related to type II radio bursts. They are thought to form sometimes as low as 2 Rs (solar radii). They are also closely linked with the acceleration of solar energetic particles.[20]
Related solar observation missionsEdit
NASA mission WindEdit
On 1 November 1994, NASA launched the Wind spacecraft as a solar wind monitor to orbit Earth's L1 Lagrange point as the interplanetary component of the Global Geospace Science (GGS) Program within the International Solar Terrestrial Physics (ISTP) program. The spacecraft is a spin axis-stabilized satellite that carries eight instruments measuring solar wind particles from thermal to >MeV energies, electromagnetic radiation from DC to 13 MHz radio waves, and gamma-rays. Though the Wind spacecraft is over two decades old, it still provides the highest time, angular, and energy resolution of any of the solar wind monitors. It continues to produce relevant research as its data has contributed to over 150 publications since 2008 alone.[citation needed]
NASA mission STEREOEdit
On 25 October 2006, NASA launched STEREO, two near-identical spacecraft which, from widely separated points in their orbits, are able to produce the first stereoscopic images of CMEs and other solar activity measurements. The spacecraft orbit the Sun at distances similar to that of Earth, with one slightly ahead of Earth and the other trailing. Their separation gradually increased so that after four years they were almost diametrically opposite each other in orbit.[21][22]
NASA mission Parker Solar ProbeEdit
The Parker Solar Probe was launched on 12 August 2018 to measure the mechanisms which accelerate and transport energetic particles i.e. the origins of the solar wind.
First tracesEdit
The largest recorded geomagnetic perturbation, resulting presumably from a CME, coincided with the first-observed solar flare on 1 September 1859. The resulting solar storm of 1859 is now referred to as the Carrington Event. The flare and the associated sunspots were visible to the naked eye (both as the flare itself appearing on a projection of the Sun on a screen and as an aggregate brightening of the solar disc), and the flare was independently observed by English astronomers R. C. Carrington and R. Hodgson. The geomagnetic storm was observed with the recording magnetograph at Kew Gardens. The same instrument recorded a crochet, an instantaneous perturbation of Earth's ionosphere by ionizing soft X-rays. This could not easily be understood at the time because it predated the discovery of X-rays by Röntgen and the recognition of the ionosphere by Kennelly and Heaviside. The storm took down parts of the recently created US telegraph network, starting fires and shocking some telegraph operators.[11]
Historical records were collected and new observations recorded in annual summaries by the Astronomical Society of the Pacific between 1953 and 1960.[23]
First clear detectionsEdit
The first detection of a CME as such was made on 14 December 1971, by R. Tousey (1973) of the Naval Research Laboratory using the seventh Orbiting Solar Observatory (OSO-7).[24] The discovery image (256 × 256 pixels) was collected on a Secondary Electron Conduction (SEC) vidicon tube, transferred to the instrument computer after being digitized to 7 bits. Then it was compressed using a simple run-length encoding scheme and sent down to the ground at 200 bit/s. A full, uncompressed image would take 44 minutes to send down to the ground. The telemetry was sent to ground support equipment (GSE) which built up the image onto Polaroid print. David Roberts, an electronics technician working for NRL who had been responsible for the testing of the SEC-vidicon camera, was in charge of day-to-day operations. He thought that his camera had failed because certain areas of the image were much brighter than normal. But on the next image the bright area had moved away from the Sun and he immediately recognized this as being unusual and took it to his supervisor, Dr. Guenter Brueckner,[25] and then to the solar physics branch head, Dr. Tousey. Earlier observations of coronal transients or even phenomena observed visually during solar eclipses are now understood as essentially the same thing.
1989-presentEdit
On 9 March 1989 a coronal mass ejection occurred. On 13 March 1989 a severe geomagnetic storm struck the Earth. It caused power failures in Quebec, Canada and short-wave radio interference.
On 1 August 2010, during solar cycle 24, scientists at the Harvard–Smithsonian Center for Astrophysics (CfA) observed a series of four large CMEs emanating from the Earth-facing hemisphere of the Sun. The initial CME was generated by an eruption on 1 August that was associated with NOAA Active Region 1092, which was large enough to be seen without the aid of a solar telescope. The event produced significant aurorae on Earth three days later.
On 23 July 2012, a massive, and potentially damaging, solar superstorm (solar flare, CME, solar EMP) occurred but missed Earth[26][27], an event that many scientists consider to be Carrington-class event.
On 31 August 2012 a CME connected with Earth's magnetic environment, or magnetosphere, with a glancing blow causing aurora to appear on the night of 3 September.[28][29] Geomagnetic storming reached the G2 (Kp=6) level on NOAA's Space Weather Prediction Center scale of geomagnetic disturbances.[30][31]
14 October 2014 ICME was photographed by the Sun-watching spacecraft PROBA2 (ESA), Solar and Heliospheric Observatory (ESA/NASA), and Solar Dynamics Observatory (NASA) as it left the Sun, and STEREO-A observed its effects directly at 1 AU. ESA's Venus Express gathered data. The CME reached Mars on 17 October and was observed by the Mars Express, MAVEN, Mars Odyssey, and Mars Science Laboratory missions. On 22 October, at 3.1 AU, it reached comet 67P/Churyumov–Gerasimenko, perfectly aligned with the Sun and Mars, and was observed by Rosetta. On 12 November, at 9.9 AU, it was observed by Cassini at Saturn. The New Horizons spacecraft was at 31.6 AU approaching Pluto when the CME passed three months after the initial eruption, and it may be detectable in the data. Voyager 2 has data that can be interpreted as the passing of the CME, 17 months after. The Curiosity rover's RAD instrument, Mars Odyssey, Rosetta and Cassini showed a sudden decrease in galactic cosmic rays (Forbush decrease) as the CME's protective bubble passed by.[32][33]
Future riskEdit
According to a report published in 2012 by physicist Pete Riley of Predictive Science Inc., the chance of Earth being hit by a Carrington-class storm between 2012 and 2022 is 12%.[26][34]
Stellar coronal mass ejectionsEdit
There have been a small number of CMEs observed on other stars, all of which as of 2016[update] have been found on M dwarfs.[35] These have been detected by spectroscopy, most often by studying Balmer lines: the material ejected toward the observer causes asymmetry in the blue wing of the line profiles due to Doppler shift.[36] This enhancement can be seen in absorption when it occurs on the stellar disc (the material is cooler than its surrounding), and in emission when it is outside the disc. The observed projected velocities of CMEs range from ≈84 to 5,800 km/s (52 to 3,600 mi/s).[37][38] Compared to activity on the Sun, CME activity on other stars seems to be far less common.[36][39]
Astronomy portal
Solar System portal
Space portal
Star portal
Forbush decrease
Health threat from cosmic rays
K-index
List of coronal mass ejections
List of solar storms
Magnetic cloud
Orbiting Solar Observatory
Solar and Heliospheric Observatory
^ Christian, Eric R. (5 March 2012). "Coronal Mass Ejections". NASA/Goddard Space Flight Center. Retrieved 9 July 2013.
^ Hathaway, David H. (14 August 2014). "Coronal Mass Ejections". NASA/Marshall Space Flight Center. Retrieved 7 July 2016.
^ "Coronal Mass Ejections". NOAA/Space Weather Prediction Center. Retrieved 7 July 2016.
^ Fox, Nicky. "Coronal Mass Ejections". NASA/International Solar-Terrestrial Physics. Retrieved 6 April 2011.
^ Gleber, Max (21 September 2014). "CME Week: The Difference Between Flares and CMEs". NASA. Retrieved 7 July 2016.
^ "Scientists unlock the secrets of exploding plasma clouds on the sun". Eurekalert.org. American Physical Society. 8 November 2010. Retrieved 7 July 2016.
^ Phillips, Tony, ed. (1 March 2001). "Cannibal Coronal Mass Ejections". Science News. NASA. Retrieved 20 March 2015.
^ Green, Lucie (2014). 15 Million Degrees. Viking. p. 212. ISBN 0-670-92218-8.
^ Holman, Gordon D. (April 2006). "The Mysterious Origins of Solar Flares". Scientific American. 294 (4): 38–45. Bibcode:2006SciAm.294d..38H. doi:10.1038/scientificamerican0406-38. PMID 16596878.
^ Baker, Daniel N.; et al. (2008). Severe Space Weather Events—Understanding Societal and Economic Impacts: A Workshop Report. National Academies Press. p. 77. doi:10.17226/12507. ISBN 978-0-309-12769-1. These assessments indicate that severe geomagnetic storms pose a risk for long-term outages to major portions of the North American grid. John Kappenman remarked that the analysis shows "not only the potential for large-scale blackouts but, more troubling, ... the potential for permanent damage that could lead to extraordinarily long restoration times."
^ a b Morring, Jr., Frank (14 January 2013). "Major Solar Event Could Devastate Power Grid". Aviation Week & Space Technology. pp. 49–50. But the most serious potential for damage rests with the transformers that maintain the proper voltage for efficient transmission of electricity through the grid.
^ Carroll, Bradley W.; Ostlie, Dale A. (2007). An Introduction to Modern Astrophysics. San Francisco: Addison-Wesley. p. 390. ISBN 0-8053-0402-9.
^ Tomczak, M.; Chmielewska, E. (March 2012). "A Catalog of Solar X-Ray Plasma Ejections Observed by the Soft X-Ray Telescope on Board Yohkoh". The Astrophysical Journal Supplement Series. 199 (1). 10. arXiv:1201.1040. Bibcode:2012ApJS..199...10T. doi:10.1088/0067-0049/199/1/10.
^ Andrews, M. D. (December 2003). "A Search for CMEs Associated with Big Flares". Solar Physics. 218 (1): 261–279. Bibcode:2003SoPh..218..261A. doi:10.1023/B:SOLA.0000013039.69550.bf.
^ Manoharan, P. K. (May 2006). "Evolution of Coronal Mass Ejections in the Inner Heliosphere: A Study Using White-Light and Scintillation Images". Solar Physics. 235 (1–2): 345–368. Bibcode:2006SoPh..235..345M. doi:10.1007/s11207-006-0100-y.
^ Freiherr von Forstner, Johan L.; Guo, Jingnan; Wimmer-Schweingruber, Robert F.; et al. (January 2018). "Using Forbush Decreases to Derive the Transit Time of ICMEs Propagating from 1 AU to Mars". Journal of Geophysical Research: Space Physics. 123 (1): 39–56. arXiv:1712.07301. Bibcode:2018JGRA..123...39F. doi:10.1002/2017JA024700.
^ Richardson, I. G. (October 2014). "Identification of Interplanetary Coronal Mass Ejections at Ulysses Using Multiple Solar Wind Signatures". Solar Physics. 289 (10): 3843–3894. Bibcode:2014SoPh..289.3843R. doi:10.1007/s11207-014-0540-8.
^ Wilkinson, John (2012). New Eyes on the Sun: A Guide to Satellite Images and Amateur Observation. Springer. p. 98. ISBN 978-3-642-22838-4.
^ Vourlidas, A.; Wu, S. T.; Wang, A. H.; Subramanian, P.; Howard, R. A. (December 2003). "Direct Detection of a Coronal Mass Ejection-Associated Shock in Large Angle and Spectrometric Coronagraph Experiment White-Light Images". The Astrophysical Journal. 598 (2): 1392–1402. arXiv:astro-ph/0308367. Bibcode:2003ApJ...598.1392V. doi:10.1086/379098.
^ Manchester, W. B., IV; Gombosi, T. I.; De Zeeuw, D. L.; Sokolov, I. V.; Roussev, I. I.; et al. (April 2005). "Coronal Mass Ejection Shock and Sheath Structures Relevant to Particle Acceleration" (PDF). The Astrophysical Journal. 622 (2): 1225–1239. Bibcode:2005ApJ...622.1225M. doi:10.1086/427768. Archived from the original (PDF) on 5 February 2007.
^ "Spacecraft go to film Sun in 3D". BBC News. 26 October 2006.
^ "STEREO". NASA.
^ Astronomical Society of the Pacific Visual Records
Nicholson, Seth B. (1954). "Solar Activity in 1953". Publications of the Astronomical Society of the Pacific. 66 (389): 55–57. Bibcode:1954PASP...66...55N. doi:10.1086/126653. ISSN 0004-6280. JSTOR 40672795.
Cragg, Thomas A. (1955). "Solar Activity in 1954". Publications of the Astronomical Society of the Pacific. 67 (395): 99–101. Bibcode:1955PASP...67...99C. doi:10.1086/126771. ISSN 0004-6280. JSTOR 40672921.
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Cragg, Thomas A. (1957). "Solar Activity in 1956". Publications of the Astronomical Society of the Pacific. 69 (407): 166–168. Bibcode:1957PASP...69..166C. doi:10.1086/127038. ISSN 0004-6280. JSTOR 40676393.
^ Howard, Russell A. (October 2006). "A Historical Perspective on Coronal Mass Ejections" (PDF). Solar Eruptions and Energetic Particles. Geophysical Monograph Series. 165. American Geophysical Union. Bibcode:2006GMS...165....7H. doi:10.1029/165GM03.
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Internet articles
Bell, Trudy E.; Phillips, Tony (6 May 2008). "A Super Solar Flare". Science@NASA. NASA.
Lavraud, Benoit; Masson, Arnaud (21 November 2007). "Cluster captures the impact of CMEs". European Space Agency.
Morring, Frank, Jr. (14 January 2013). "Major Solar Event Could Devastate Power Grid". Aviation Week & Space Technology.
Odenwald, Sten F.; Green, James L. (28 July 2008). "Bracing the Satellite Infrastructure for a Solar Superstorm". Scientific American.
Phillips, Tony (27 May 2008). "Cartwheel Coronal Mass Ejection". Science@NASA. NASA.
Wikimedia Commons has media related to Coronal mass ejection.
NOAA/NWS Space Weather Prediction Center
Coronal Mass Ejection FAQ
STEREO and SOHO observed CME rate versus the Sunspot number (PNG plot) / (text version)
Retrieved from "https://en.wikipedia.org/w/index.php?title=Coronal_mass_ejection&oldid=903239402"


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which are 105 of 535 seats between the Senate and the House of Representatives.
The good thing is that we can work to improve it in the next year. All the
remaining Senate will be up for election.
Are More Likely to Live in Poverty
Women's Law Cent said that 12.5% of the women in the United States of America
are living in poverty in 2016, at total of 16.9 million people. One in three
single mothers in the US are living in poverty, and the kids affected to, with
56.2 percent of kids living in poverty.
Gender Equality Is Getting Worse
United States of America in 2006 took the third place for economic gender
equality but in 2016 it dropped to the twenty sixth place. A very strange
change in a ten years only. According to the World Economic Forum, women should
be the one that may leave the work not the men.
Pay More 42% Of The Time
was a video released by |Glamor last year, "The cost of being a woman" focus on
product that women are paying more for it then men. For example, deodorant was
$5.99 for women and $3.29 for men. In 2016 consumer affairs management decided
that women are paying for their version 42 percent more then men of products
which it now called "pink tax". It is gets in all the areas in women's lives.
In 2012 Bic released a line of pen which in pink and purple especially for
women; it is exactly similar of other pens beside the color but its sold with a
double prices then the other pens. Asking Ellen DeGeneres to be their
spokesperson was a mistake that Bic made because she tore them a little in a
fake advertisement, saying that the packaging designed to fit women's hands.
10 Million Women a Year Are Victims of Domestic Violence
in houses is speeded in America, beside it includes men also. But it
concentrates women the most. The scariest thing that three women are being
killed by their friends or husbands. While Obama's plan doing a huge step to
get rid of violence and trying to help the people who suffers from it. On the
other hand, Tramp has signed an executive order "Enhance Public Safety Interior
Of The United States". According to Tahira Justice Center this order may not
authorized women from coming further requesting legal safety from fear of
depuration.
Cost of Being a Woman l Glamour magazine https://www.youtube.com/watch?v=e7jfCp8sKOE
Menopause ends. Its onset is 40s and late 60s.
Dalton The United States is the land of equal
Kevin created to limit immigration was the Chinese Exclusion
Change for instance, those between human/brute and men/women. Carter's
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