diff --git a/README.md b/README.md index 4b9aa1e..7f26bfc 100644 --- a/README.md +++ b/README.md @@ -34,8 +34,9 @@ outlines the corrections and component calculation pipeline 3. [RV Calculations](https://github.com/tamarervin/sdo_hmi_rvs/blob/main/sdo_hmi_rvs/examples/rv_calculation.ipynb): outlines calculation of full model RV from velocity components - * requires input CSV with velocity components from [example 2](https://github.com/tamarervin/sdo_hmi_rvs/blob/main/sdo_hmi_rvs/examples/component_calculations.ipynb) - + * requires input CSV with velocity components from [example 2](https://github.com/tamarervin/sdo_hmi_rvs/blob/main/sdo_hmi_rvs/examples/component_calculations.ipynb) + * an example CSV file with calculations is stored [here](https://github.com/tamarervin/sdo_hmi_rvs/blob/main/sdo_hmi_rvs/products/csv_files/calcs/example_calcs.csv) + 4. [Full Pipeline](https://github.com/tamarervin/sdo_hmi_rvs/blob/main/sdo_hmi_rvs/examples/full_pipeline.ipynb): full end-to-end pipeline to calculate 'sun-as-a-star' RVs and magnetic observables diff --git a/mkdocs/docs/examples/docs_rv_calcs.ipynb b/mkdocs/docs/examples/docs_rv_calcs.ipynb index 4e28d61..96dd276 100644 --- a/mkdocs/docs/examples/docs_rv_calcs.ipynb +++ b/mkdocs/docs/examples/docs_rv_calcs.ipynb @@ -7,7 +7,11 @@ "\n", "1. **calculate solar velocities:** calculate solar velocities and save to csv\n", "2. **get component lists:** using pandas to get the lists of each relevant component\n", - "3. **calculate RVs and save to csv:** calculate RVs using optimized parameters" + "3. **calculate RVs and save to csv:** calculate RVs using optimized parameters\n", + "\n", + "\n", + "**NOTE:** this is purely an example but requires ground-based Solar RV\n", + "measurements for fitting" ], "metadata": { "collapsed": false diff --git a/mkdocs/docs/examples/docs_solar_corrections.ipynb b/mkdocs/docs/examples/docs_solar_corrections.ipynb index dcff774..289def0 100644 --- a/mkdocs/docs/examples/docs_solar_corrections.ipynb +++ b/mkdocs/docs/examples/docs_solar_corrections.ipynb @@ -482,7 +482,8 @@ "execution_count": null, "outputs": [], "source": [ - "map_int_cor = [sfuncs.corrected_map(Iflat[i], hmi_int[i], map_type='Corrected-Intensitygram', frame=frames.HeliographicCarrington) for i in range(0, len(hmi_int))]" + "map_int_cor = [sfuncs.corrected_map(Iflat[i], hmi_int[i], map_type='Corrected-Intensitygram',\n", + " frame=frames.HeliographicCarrington) for i in range(0, len(hmi_int))]" ], "metadata": { "collapsed": false, diff --git a/mkdocs/site/examples/docs_solar_corrections/index.html b/mkdocs/site/examples/docs_solar_corrections/index.html index 007ac5d..472498c 100644 --- a/mkdocs/site/examples/docs_solar_corrections/index.html +++ b/mkdocs/site/examples/docs_solar_corrections/index.html @@ -1692,8 +1692,8 @@
Apply coordinate transformations for HMI data products where:
-x, y, pd, r, d, mu = coord[i][0], coord[i][1], coord[i][2], coord[i][3], coord[i][4], coord[i][5]
wij, nij, rij = vel_coords[i][0], vel_coords[i][1], vel_coords[i][2]
x, y, pd, r, d, mu = coord[i][0], coord[i][1], coord[i][2], coord[i][3], coord[i][4], coord[i][5]
wij, nij, rij = vel_coords[i][0], vel_coords[i][1], vel_coords[i][2]
Remove bad mu values from each map.
-hmi_vel, hmi_mag, imap = maps[i][0], maps[i][1], maps[i][2]
hmi_vel, hmi_mag, imap = maps[i][0], maps[i][1], maps[i][2]
Calculate relative positions.
-deltaw, deltan, deltar, dij = delta[i][0], delta[i][1], delta[i][2], delta[i][3]
deltaw, deltan, deltar, dij = delta[i][0], delta[i][1], delta[i][2], delta[i][3]
We calculate radial unsigned magnetic field strength and set pixels with an observed magnetic field below the noise value equal to zero.
The noise level used is from Yeo et al. 2013, and is 8 Gauss.
-Bobs, Br = corrected_mag[0], corrected_mag[1]
Bobs, Br = corrected_mag[0], corrected_mag[1]
For weighting, we return an active weights array (active = 1) and quiet weights array (active = 0).
Get threshold maps where:
-active, quiet = mag_thresh[i][0], mag_thresh[i][1]
active, quiet = mag_thresh[i][0], mag_thresh[i][1]
Calculate intensity threshold value and differentiate between sunspots and faculae where:
-fac_inds, spot_inds = int_thresh[0], int_thresh[1]
fac_inds, spot_inds = int_thresh[0], int_thresh[1]
Calculate photometric velocity.
-v_phot, vphot_bright, vphot_spot = vphot[0], vphot[1], vphot[2]
v_phot, vphot_bright, vphot_spot = vphot[0], vphot[1], vphot[2]
Estimate the disc-averaged filling factors of sunspots and plage: $ f_{spot, plage} = \frac{1}{N_{pix}} \sum_{ij} W_{ij} $
In this case, a weight of 1 is an active pixel (active_weights).
-f_bright, f_spot, f = filling[0], filling[1], filling[2]
f_bright, f_spot, f = filling[0], filling[1], filling[2]
Calculate the area filling factor.
-f_small, f_large, f_network, f_plage, f_nonconv = f_area[0], f_area[1], f_area[2], f_area[3], f_area[4]
f_small, f_large, f_network, f_plage, f_nonconv = f_area[0], f_area[1], f_area[2], f_area[3], f_area[4]
Calculate unsigned flux of various polarized and active regions.
-quiet_flux, ar_flux, conv_flux, pol_flux, pol_conv_flux = flux[0], flux[1], flux[2], flux[3], flux[4], flux[5]
quiet_flux, ar_flux, conv_flux, pol_flux, pol_conv_flux = flux[0], flux[1], flux[2], flux[3], flux[4], flux[5]
Get area weighted convective velocities.
-vconv_quiet, vconv_large, vconv_small = vconv_area[0], vconv_area[1], vconv_area[2]
vconv_quiet, vconv_large, vconv_small = vconv_area[0], vconv_area[1], vconv_area[2]