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Sökning: onr:"swepub:oai:DiVA.org:su-145851" > Orbital Elements an...

LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00003576naa a2200517 4500
001oai:DiVA.org:su-145851
003SwePub
008170823s2017 | |||||||||||000 ||eng|
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1458512 URI
0247 a https://doi.org/10.3847/1538-4357/aa7b872 DOI
040 a (SwePub)su
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Hummel, C. A.4 aut
2451 0a Orbital Elements and Stellar Parameters of the Active Binary UX Arietis
264 c 2017-07-28
264 1b American Astronomical Society,c 2017
338 a print2 rdacarrier
520 a Stellar activity observed as large surface spots, radio flares, or emission lines is often found in binary systems. UX Arietis exhibits these signs of activity, originating on the K0 subgiant primary component. Our aim is to resolve the binary, measure the orbital motion, and provide accurate stellar parameters such as masses and luminosities to aid in the interpretation of the observed phenomena. Using the CHARA six-telescope optical long-baseline array on Mount Wilson, California, we obtained amplitudes and phases of the interferometric visibility on baselines up to 330 m in length, resolving the two components of the binary. We reanalyzed archival Center for Astrophysics spectra to disentangle the binary component spectra and the spectrum of the third component, which was resolved by speckle interferometry. We also obtained new spectra with the Nordic Optical Telescope, and we present new photometric data that we use to model stellar surface spot locations. Both interferometric visibilities and spectroscopic radial velocities are modeled with a spotted primary stellar surface using the Wilson-Devinney code. We fit the orbital elements to the apparent orbit and radial velocity data to derive the distance (52.1 +/- 0.8 pc) and stellar masses (M-P = 1.30 +/- 0.06 M-circle dot, M-S = 1.14 +/- 0.06 M-circle dot). The radius of the primary can be determined to be R-P = 5.6 +/- 0.1 R-circle dot and that of the secondary to be R-S = 1.6 +/- 0.2 R-circle dot. The equivalent spot coverage of the primary component was found to be 62% with an effective temperature 20% below that of the unspotted surface.
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
653 a binaries: spectroscopic
653 a stars: activity
653 a stars: individual (UX Ari)
653 a stars: late-type
653 a starspots
7001 a Monnier, J. D.4 aut
7001 a Roettenbacher, Rachael M.u Stockholms universitet,Institutionen för astronomi4 aut0 (Swepub:su)rroet
7001 a Torres, G.4 aut
7001 a Henry, G. W.4 aut
7001 a Korhonen, H.4 aut
7001 a Beasley, A.4 aut
7001 a Schaefer, G. H.4 aut
7001 a Turner, N. H.4 aut
7001 a Ten Brummelaar, T.4 aut
7001 a Farrington, C. D.4 aut
7001 a Sturmann, J.4 aut
7001 a Sturmann, L.4 aut
7001 a Baron, F.4 aut
7001 a Kraus, S.4 aut
7102 a Stockholms universitetb Institutionen för astronomi4 org
7730 t Astrophysical Journald : American Astronomical Societyg 844:2q 844:2x 0004-637Xx 1538-4357
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-145851
8564 8u https://doi.org/10.3847/1538-4357/aa7b87

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