Making quick-look flare spectrograms and movies

This page documents instructions for EOVSA Scientists-on-Duty (SoD) to create quicklook flare spectrograms and movies as part of their daily routines.

Producing EOVSA quick-look flare spectrograms

Step 1: Checking Possible flares

Verify the possible flares on the daily EOVSA Solar Dynamic Spectrogram, for example:

http://ovsa.njit.edu/browser/?suntoday_date=2024-05-07

In this example, we see a possible flare that happened around 16:30 UT, which appears as a bright vertical stripe in the daily cross-power dynamic spectrum.

For better visualization and flare time precision, check the higher-resolution dynamic spectra at:

http://ovsa.njit.edu/flaremon/. "XSPYYYYMMDDHHMMSS.png" are the file names you are looking for.

Since 2024-May-05, real-time flare detection figures and list are also available at:

http://ovsa.njit.edu/flaremon/FLM20240507.png http://ovsa.njit.edu/flaremon/flarelist/flarelist_2024-05-07.txt

Step 2: Set up the environment

Login into the pipeline machine with your account:

ssh -X [your_user_name]@pipeline

If your default shell is not bash, enter bash by

bash

If the following is not already in your ~/.bashrc file, do the following

alias loadpyenv3.8='source /home/user/.setenv_pyenv38'
export EOVSADBJSON=/common/python/current/EOVSADB.json 

Enter a working directory. We have limited space under /home, so it is better to go to your directory under /data1/.

cd /data1/<your_user_name>/

Load the Python 3.8 environment

loadpyenv3.8
ipython --pylab

In Python, enter the following:

from eovsapy import flare_spec as fs 
from eovsapy.util import Time 

Step 3: Analyze the flare

Obtain IDB files by providing a time range that encloses the flare. This step will also perform various calibration steps (absolute flux, attenuator gain, and feed rotation), so it may take a long while (~hour depending on your flare duration). During the course, it will also ask you to confirm the files to be processed. Each IDB file is supposed to be 10-minute long. The naming convention is "IDByyyymmddhhmmdd," with the time indicating the start time of the file.

The timerange corresponds to these files (will take about 8 minutes to process)
/data1/eovsa/fits/IDB/20240507/IDB20240507162024
/data1/eovsa/fits/IDB/20240507/IDB20240507163024
Do you want to continue? (say no if you want to adjust timerange) [y/n]?y 

files = fs.calIDB(Time(['2024-05-07 16:20','2024-05-07 16:35'])) 

The previous step, if successful, will produce a list of IDB files under the current directory

In [21]: print(files)
['./IDB20240507162024', './IDB20240507163024']

Inspect the spectrograms and see if all the antennas look okay.

out, spec = fs.inspect(files) 

But, if one or more antennas are known to be working, enter the list of the good ones. In this example, we have antennas 7 and 10 that were being serviced at the time. So let us exclude them using the "ant_str" parameter. Note the antenna names go from 1 to 13.

 out, spec = fs.inspect(files, ant_str='ant1-6 ant8-9 ant11-13') 

To better see the flare, you can change the spec vmax as:

 imshow(spec,vmax=30,vmin=-1) 

Use the figure above to choose the background interval (bgidx), the maximum intensity and the frequencies.

The tpk (Time of the peak) determines the name of the resulting files (.png and .fits), and also determines the flare_id.

It's better to keep the formate of tpk as tpk='yyyy-mm-dd hh:mm:00' and add the flare time on wiki in the format of "hh:mm":

 f, ax0, ax1 = fs.make_plot(out,bgidx=[200,210],vmin=0.1, vmax=110, lcfreqs=[120,190,270,350],ant_str='ant1-6 ant8-9 ant11-13', tpk='2024-05-07 16:30:00') 

A second background interval can be defined right after the first one, e.g., bg2idx=[1000,1010]

In this example, the output files are eovsa.spec.flare_id_20240507163000.fits and eovsa.spec.flare_id_20240507163000.fits.

At the end, copy the .fits file to /common/webplots/events/2024:

 cp eovsa.spec.flare_id_20240507163000.fits /common/webplots/events/2024 

and include the flare in the wiki Flare List:

http://ovsa.njit.edu/wiki/index.php/2024

The flare position have been copied from the https://solarmonitor.org/