E-Print Archive

There are 4249 abstracts currently viewable.


Search:

Advanced Search
Options
Main Page Add New E-Print Submitter
Information
Feedback
News Help/FAQ About Preferences
Manage Key Phrase
Notification
* News 04/04/20 * The archive is using a new backend database. This has thrown up a few SQL errors in the last few days. If you have any issues please email adavey@nso.edu with either the number of eprint you are trying to edit or a link to your preprint.

Response of SDO/HMI observables to heating of the solar atmosphere by precipitating high-energy electrons View all abstracts by submitter

Viacheslav Sadykov   Submitted: 2020-03-06 13:15

We perform an analysis of the line-of-sight (LOS) observables of the SDO/HMI for models of the solar atmosphere heated by precipitating high-energy electrons during solar flares. The radiative hydrodynamic (RADYN) flare models are obtained from the F-CHROMA database. The Stokes profiles for the Fe 6173 Å line observed by SDO/HMI are calculated using the radiative transfer code RH1.5D assuming statistical equilibrium for atomic level populations and imposing uniform background vertical magnetic field of various strength. The SDO/HMI observing sequence and LOS data processing pipeline algorithm are applied to derive the observables (continuum intensity, line depth, Doppler velocity, LOS magnetic field). Our results reveal that the strongest deviations of the observables from the actual spectroscopic line parameters are found for the model with a total energy deposited of Etotal=1.0x1012 erg cm-2, injected with power-law spectral index of δ=3 above a low-energy cutoff of Ec=25 keV. The magnitudes of the velocity and magnetic field deviations depend on the imposed magnetic field, and can reach 0.35 km s-1 for LOS velocities, 90 G for LOS magnetic field, and 3% for continuum enhancement for the 1000 G imposed LOS magnetic field setup. For Etotal≥3.0x1011 erg cm-2 models, the velocity and magnetic field deviations are most strongly correlated with the energy flux carried by ~50 keV electrons, and the continuum enhancement is correlated with the synthesized ~55-60 keV hard X-ray photon flux. The relatively low magnitudes of perturbations of the observables and absence of magnetic field sign reversals suggest that the considered radiative hydrodynamic beam heating models augmented with the uniform vertical magnetic field setups cannot explain strong transient changes found in the SDO/HMI observations.

Authors: Viacheslav M Sadykov, Alexander G Kosovichev, Irina N Kitiashvili, Graham S Kerr
Projects: SDO-HMI

Publication Status: Accepted to ApJ
Last Modified: 2020-03-07 09:29
Go to main E-Print page  Can Sub-photospheric Magnetic Reconnection Change the Elemental  Composition in the Solar Corona?  3He-Rich Solar Energetic Particles: Solar Sources  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

Key
Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
Ambipolar diffusion in the Bifrost code
Modeling the quiet Sun cell and network emission with ALMA
Clustering of fast Coronal Mass Ejections during the solar cycles 23 and 24 and implications for CME-CME interactions
Magnetic and Velocity Field Topology in Active Regions of Descending Phase of the Solar Cycle 23
Numerical simulation of solar photospheric jet-like phenomena caused by magnetic reconnection
Solar Flare-CME Coupling Throughout Two Acceleration Phases of a Fast CME
A new method for estimating global coronal wave properties from their interaction with solar coronal holes
Machine-learning approach to identification of coronal holes in solar disk images and synoptic maps
Multilevel Observations of the Oscillations in the First Active Region of the New Cycle
Standing MHD Waves in a Magnetic Slab Embedded in an Asymmetric Magnetic Plasma Environment: Surface Waves
A new facility for airborne solar astronomy: NASA's WB-57 at the 2017 total solar eclipse
MinXSS-2 CubeSat mission overview: Improvements from the successful MinXSS-1 mission
Lyman α Variability During Solar Flares Over Solar Cycle 24 Using GOES-15/EUVS-E
Sunquake with a second-bounce, other sunquakes and emission associated with X9.3 flare of 6 September 2017. II. Proposed interpretation
f-mode strengthening from a localized bipolar subsurface magnetic field
Imaging and spectral study on the null point of a fan-spine structure during a solar flare
Forecasting Solar Cycle 25 Using Deep Neural Networks
An Observational Test of Solar Plasma Heating by Magnetic Flux Cancellation
The Drivers of Active Region Outflows into the Slow Solar Wind
HXR emission from an activated flux rope and subsequent evolution of an eruptive long duration solar flare

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey



© 2000-2020 Solar Physics Group - Montana State University