Done, Done, and We’re on to the Next One!
The first round of Sunspotter data classification has been completed!
It took around 1,639 registered volunteers (+ an unknown number of anonymous volunteers) 324,465 clicks to compare each image in the set of 12,966 data at least 50 times. So thats an average of 198 clicks/registered volunteer!
Of course in reality, there are those few Sunspotter-aholics that probably did a lion’s share of the work- To everyone that wants to get going on comparing the next set of images, we are working as fast as possible to get the next set of data up!
The forthcoming dataset relies on sunspot groups detected by a completely automated algorithm (not relying on human intervention, like the last dataset), called the SolarMonitor Active Region Tracker (SMART; Higgins et al. 2011), and will not be prone to human bias. It will include over two hundred thousand images of sunspot groups. A number of the sunspot groups will overlap with the last dataset, but will be detected and processed in a different way.
As mentioned in a previous post we are using ‘Stereographic Projection‘ techniques to ‘de-smoosh’ the sunspot groups near the solar limb (edge), so that they appear as if they were at the center of the Sun. Stereographic projections are rarely used for images of the Sun (if anyone knows of an example, please tell me!), but they are common in astrophysics). Also, they are commonly used to make maps of the South and North pole of the Earth because although features at the edge of the map become larger by a factor of ~2, they keep shapes the same (the more usual Mercator maps completely distort shape near the poles). Keeping shape the same, or being conformal, is important for Sunspotter, because the shape of a sunspot group is likely to have a big effect on apparent complexity!
In addition to being the first time that anyone has measured the ‘true’ complexity of a large sample sunspot groups, we will now be able to measure the evolution ofsunspot group complexity, and determine how that relates to eruptions.
In the mean time, we will be analysing the previous dataset to determine how complexity relates to other properties of sunspot groups and to solar flare occurrence. Exciting times!