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. Attached Files Name Description MIMEType Size Downloads Title Stellar surface magneto-convection as a source of astrophysical noise. I. multi-component parameterization of absorption line profiles Author(s) Cegla, HM 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 Related Links Link Description Connect to published version Go to link with your DU access privileges     Unless expressly stated otherwise, the copyright for items in DRO is owned by the author, with all rights reserved. Versions Version Filter Type Fri, 02 Nov 2018, 14:10:38 EST Sat, 03 Nov 2018, 04:04:03 EST Wed, 20 Mar 2019, 11:25:59 EST Sat, 23 Mar 2019, 05:05:16 EST Wed, 27 Mar 2019, 09:23:24 EST Wed, 27 Mar 2019, 09:25:41 EST Wed, 27 Mar 2019, 09:26:39 EST Filtered Full Citation counts:   Cited 12 times in TR Web of Science Cited 9 times in Scopus Search Google Scholar Access Statistics: 10 Abstract Views, 4 File Downloads  -  Detailed Statistics Created: Wed, 20 Mar 2019, 11:25:59 EST

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