Stellar surface magneto-convection as a source of astrophysical noise. I. multi-component parameterization of absorption line profiles

Cegla, HM, Shelyag, Sergiy, Watson, CA and Mathioudakis, M 2013, Stellar surface magneto-convection as a source of astrophysical noise. I. multi-component parameterization of absorption line profiles, Astrophysical journal, vol. 763, no. 2, pp. 1-8, doi: 10.1088/0004-637X/763/2/95.

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Title Stellar surface magneto-convection as a source of astrophysical noise. I. multi-component parameterization of absorption line profiles
Author(s) Cegla, HM
Shelyag, SergiyORCID iD for Shelyag, Sergiy orcid.org/0000-0002-6436-9347
Watson, CA
Mathioudakis, M
Journal name Astrophysical journal
Volume number 763
Issue number 2
Article ID 95
Start page 1
End page 8
Total pages 8
Publisher IOP Publishing
Place of publication Bristol, Eng.
Publication date 2013-02-01
ISSN 0004-637X
1538-4357
Keyword(s) line: profiles
planets and satellites: detection
stars: activity
stars: low-mass
Sun: granulation
techniques: radial velocities
Science & Technology
Physical Sciences
Astronomy & Astrophysics
Summary We outline our techniques to characterize photospheric granulation as an astrophysical noise source. A four-component parameterization of granulation is developed that can be used to reconstruct stellar line asymmetries and radial velocity shifts due to photospheric convective motions. The four components are made up of absorption line profiles calculated for granules, magnetic intergranular lanes, non-magnetic intergranular lanes, and magnetic bright points at disk center. These components are constructed by averaging Fe I 6302 Å magnetically sensitive absorption line profiles output from detailed radiative transport calculations of the solar photosphere. Each of the four categories adopted is based on magnetic field and continuum intensity limits determined from examining three-dimensional magnetohydrodynamic simulations with an average magnetic flux of 200 G. Using these four-component line profiles we accurately reconstruct granulation profiles, produced from modeling 12 × 12 Mm2 areas on the solar surface, to within ∼ ±20 cm s-1 on a ∼100 m s-1 granulation signal. We have also successfully reconstructed granulation profiles from a 50 G simulation using the parameterized line profiles from the 200 G average magnetic field simulation. This test demonstrates applicability of the characterization to a range of magnetic stellar activity levels.
Language eng
DOI 10.1088/0004-637X/763/2/95
Field of Research 0201 Astronomical And Space Sciences
0305 Organic Chemistry
0306 Physical Chemistry (Incl. Structural)
HERDC Research category C1.1 Refereed article in a scholarly journal
Copyright notice ©2013, The American Astronomical Society
Persistent URL http://hdl.handle.net/10536/DRO/DU:30114957

Document type: Journal Article
Collection: School of Information Technology
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