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I am going to stick my neck out here but I wondered if observers actually calculate the obscuration of the sun by the moon from the pictures that they take of the partial eclipse or does this have no value because the earth/moon system dynamics is so well known? I think that the obscuration percentage is given by the simple formula 100(w – sin w)/pi if you assume that the sun and moon appear to be the same anglular size. If you draw a chord between the points where the moon’s shadow touches the sun’s edge (the chord PP’ in the attached diagram) the angle w (in radians) is the angle subtended by P and P’ from the centre of the sun’s image. If you have an image of the partial eclipse you can measure (in pixels) the diameter of the sun’s disc and the length of the chord l and then w = 2 arcsin (l/d).
For example, for my image of the partial eclipse taken at 09:45 UT on the 25th from 52 degrees 44 minutes north and 1 degree 28 minutes east, l was 209 pixels, d was 311 pixels and so the obscuration was about 15% at this time (this was about 15 minutes from maximum coverage).
Even if the calculation has no scientific value, it may still be interesting to calculate and compare with prediction.
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Thanks Gary. I hadn’t added myself to the BAAVSS alert group, so I have requested this now. Can the new chart 106.04 be used in the online database already?
Duncan.
Thanks Bill, that kind of makes sense that there is some kind of multiplying factor that is observer and instrumentation dependent. I was wondering how this all worked because I could see that the better the instrumentation and resolution you had, the more sunspots you might count. I haven’t tried using a Stonyhurst disc yet, that was something I was going to try and grapple with next. I think for the moment I will continue with my approach of projecting the image first and getting a handle on the basics before moving on to solar filters etc.
Thanks very much Peter, that clarifies things a lot. I hadn’t thought that it was the center of the groups that was used to determine their distance apart on the solar disk, I had just assumed that it was how close their edges were. So that helps. I also didn’t realise it was just the umbrae that counted towards the spot number, either. I think I might try and add some observations to the database that you mentioned once I get the hang of things a bit better but I notice from your newsletter that we can email images to you. Do you have any preference about whether the image is annotated in any way (e.g. with AR numbers?). I note using the time, date and initials in the file name and copying them to Lyn. Any preferred format for the file name? many thanks.
Another aspect of the light curve of this star that interested me was that from time-to-time the maxima appear to be double peaked. This has been shown nicely by some recent observations using CMOS detectors (see the attached file which has been produced from the BAA database). If you look at the light curve after the 1st Jan 2022 you can see (green data points) that Z UMa reached a maximum of about magnitude 6.6 around the 14th March, then it faded a bit to about 7.7 around the 21st April before brightening again to about magnitude 6.8 around the 22nd May (roughly 69 days from peak-to-peak). The same double peak is seen in the visual data (black circles) but the scatter in the CMOS data is much tighter. Looking back at the four maxima prior to this the visual data (black circles) hint that this double peaked behaviour has been been developing as time progresses.
If you go back further in time other reasonably clear examples of a double peak can be seen in August 2016, January 2008 to July 2009, January 1999, July 1999 and July 1995 (I haven’t gone back further than this). So what is causing this? One suggestion has been that this is due to the interaction of different pulsation cycles within the star but this is not so easy to understand if, as John Greaves says (see my first post), after 1995 there is virtually only one pulsation period of 189 days. With more people carrying out observations using more accurate electronic detectors it will be interesting to see how often this double peaked behaviour appears.
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Thanks Jeremy for all these useful links. I have had a brief look at the T UMi paper and scanned the June edition of the AGB Newsletter. People who are modelling the evolution of stars on the AGB seem very keen that we keep monitoring stars whose periods are changing over time.
Hi Lyn, this is embarrassing. I forgot to subtract an hour from my timing of my solar image I took on the 21st April. So this should read 11:07 UT not 12:07 UT. Sorry about this.
Hi Lyn, I am a new member of the BAA and thought I would try and contribute to this thread (my first post on the forum). I took this image on the 21st April at 12:07 UT using a Celestron NexStar 102SLT. I used a 25mm eyepiece and a star diagonal to project the image onto white paper. I have rotated it as best I could to give the correct orientation. There are two versions of the same image. One has the sunspot groups annotated. I hope that this is useful to you.
