Download Summerschool Projects: Project 1: Sunspot data and solar cycle

Summerschool Projects:
Project 1:
Sunspot data and solar cycle analysis (1 group):
Task 1: Get the monthly sunspot data (and smoothed sunspot data) from the SIDC (solar influence
data center: http://www.sidc.be/)
Task 2: Read the ascii file by IDL routines; split the string information and save it in various variables;
e.g.: time should be stored in two variables: a year and a month variable
sunspot data in a floating variable called rel_ss_num
Task 3: do an utplot of the sunspot number versus time;
Task 4: find the minima of the cycles and split the time series in the different cycles.
Task 5: Curvefit the different cycles with a sine function (curvefit routine) and with a polynomial (4th
order).
Task 6: write an ascii file with starting time of the cycle, maximum amplitude (from the data and the
two fits) and time of the maximum (from data and the fits).
Task 7: Estimate the mean amplitude and the mean duration of the cycles. How many cycles had
higher/lower amplitudes and durations compared to these mean values.
Task 8: Discuss the different results from the curvefits and the direct data.
Group 1:
Names (3 participiants possible):
Project 2:
Data alignment and sunspot investigation (2 groups possible):
Task 1: Find a suitable Hinode/SOT data set comprising of BFI filtergram information (blue continuum
or g-band) with inverted SP data (magnetogram).
Task 2: Download these data.
Task 3: calibrate the filtergram data (fg_prep).
Task 3: Cross align the data sets (cross_corr).
Task 4: Plot the countour of the magnetic field over the filtergram data (1000 G and 2000 G).
Task 5: Create a ps-plot of the last plot and save the image with the countours as fits file.
Task 6: Find the boundary conditions (magnetic field strength) between the umbra/penumbra and
penumbra/surrounding quiet sun.
Task 7: The same as in task 4 with these countour levels and also task 5.
Task 8: Create histograms of the magnetic field strength of the umbra and penumbra (in one plot)
and a histogram of the magnetic field inclinations of the umbra and penumbra (in one plot)
Task 9: Discuss the found difference in field strength and inclination between umbra and penumbra.
Group 2:
Names (3 participiants possible):
Group 3:
Names (3 participiants possible):
Project 3:
Goes and magnetic field (flare classification and impact on magnetic field; 2 groups possible)
Task 1: Find via the sswidl „goes“ routines a „nice“ flare event.
Task 2: Characterice the flare due to its x-ray flux and estimate the duration of the flare event.
Task 3: Find suitable magnetogram data to the flare event. Preferentially in this order inverted
Hinode/SP data, SDO/HMI data, SOHO/MDI high resolution or SOHO/MDI full disc.
Task 4: Estimate the magnetic flux in the flaring region before and after the flare.
Task 5: Get radio data (e.g. Nancay) and interpret the flare signatures.
Task 6: Get extreme ultraviolete data during the flare event (Stereo/EUV or SoHo/EIT).
Task 7: Create a movie of the flare (coronal data, EUV/EIT).
Task 8: Get the countours of the flare event (during the máximum) in the EUV/EIT and overplot these
countours on the magnetogram data.
Group 4:
Names (3 participiants possible):
Group 5:
Names (3 participiants possible):
Project 4:
Flux emergence (forming sunspot; 1 group):
Task 1: Access the data SOT/NFI & SOT/BFI from (case I):
http://msslxr.mssl.ucl.ac.uk:8080/eiswiki/Wiki.jsp?page=FluxData
Task 2: Assume that the magnetic field strength ranges from 0 to 2000 G for the existing sunspot
(bright polarity). Use this information to scale also the dark polarity.
Task 3: As soon as the sunspot gets visible in the BFI data, threshold the sunspot and estimate the
total magnetic flux of the sunspot (field strength times size). Also plot the countours of the sunspot
in the NFI data.
Task 4: Do this for the complete time series and investigate how the magnetic flux is changing with
time.
Task 5: Estimate the time span it needs to form the sunspot.
Task 6: Create a movie of the NFI data as well as of the BFI data.
Task 7: Measure the center position of both sunspots (corrected for solar B angle (hint pb0r)).
Task 8: Estimate in all images the distance between the center of the newly formed sunspot to the
center of the old sunspot.
Task 9: Calculate the velocity with which the sunspots are closing up. Plot the evolution of this
velocity with time and save it as ps-plot.
Task 10: Discuss why the newly formed sunspot moves.
Group 6:
Names (3 participiants possible):
Project 5:
CME propagation:
Task 1: Find a proper CME event.
Task 2: Search for datasets within the STEREO and SOHO mission (Cor 1,2, HI 1,2, of A & B spacecraft
and SOHO/LASCO C2 & C3)
Task 3: Calibrate the data.
Task 4: Make movies of the CME seen from the 3 spacecrafts and hence vantage points.
Task 5: Discuss why the CME appears different in the 3 spacecrafts.
Task 6: Estimate the CME front (position)
Task 7: Calculate the velocity of the CME and plot the velocity/time diagram.
Task 8: Create J-plots.
Task 9: Infere the velocity of the CME out of the J-plot.
Group 7:
Names (3 participiants possible):
Project 6:
Investigating the CLV (center to limb variation) and the differential rotation:
Task 1: Get synoptic full disc images and derive the center to limb variation of intensity in different
wavelengths (e.g. Kanzelhöhe: whitelight, Hα, Ca II).
Task 2: Fit the CLV with a polynomial function.
Task 3: Discuss why (if) the CLV is different for different wavelengths. What causes the CLV?
Task 4: Try to calibrate a monthly synoptic data set (dividing the images by the CLV, so that the
contrast/brightness seems to be flat).
Task 5: Derive the position of an active group (thresholding of the image). Follow the active group
during one rotation and estimate the rotation periode of the Sun.
Task 6: Repeat this for different periods during the solar cycle (e.g. every year/half year when
sunspots are visible). The sunspots should move from the beginning of the cycle (~40° latitude) closer
to the equator (during the end ~10°). Hence you can estimate the differential rotation of the surface
of the Sun for those latitudes.
Task 7: Discuss how and if it is possible to estimate the differential rotation for other latitudes.
Group 8:
Names (3 participiants possible):