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Sökning: (WFRF:(Curto M)) srt2:(2005-2009) > (2007) > Pulsation in the at...

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FältnamnIndikatorerMetadata
00003675naa a2200529 4500
001oai:DiVA.org:uu-14075
003SwePub
008080128s2007 | |||||||||||000 ||eng|
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-140752 URI
0247 a https://doi.org/10.1051/0004-6361:200663652 DOI
040 a (SwePub)uu
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Ryabchikova, T.4 aut
2451 0a Pulsation in the atmosphere of the roAp star HD 24712 :b I. Spectroscopic observations and radial velocity measurements
264 c 2006-11-13
264 1b EDP Sciences,c 2007
338 a print2 rdacarrier
520 a Aims.We have investigated the structure of the pulsating atmosphere of one of the best studied rapidly oscillating Ap stars, HD 24712.Methods.For this purpose we analyzed spectra collected during 2001-2004. An extensive data set was obtained in 2004 simultaneously with the photometry of the Canadian MOST mini-satellite. This allows us to connect directly atmospheric dynamics observed as radial velocity variations with light variations seen in photometry. Results.We directly derived for the first time and for different chemical elements, respectively ions, phase shifts between photometric and radial velocity pulsation maxima indicating, as we suggest, different line formation depths in the atmosphere. This allowed us to estimate for the first time the propagation velocity of a pulsation wave in the outer stellar atmosphere of a roAp star to be slightly lower than the sound speed. We confirm large pulsation amplitudes (150-400 m s-1) for REE lines and the H core, while spectral lines of the other elements (Mg, Si, Ca, and Fe-peak elements) have nearly constant velocities. We did not find different pulsation amplitudes and phases for the lines of rare-earth elements before and after the Balmer jump, which supports the hypothesis of REE concentration in the upper atmosphere above the hydrogen line-forming layers. We also discuss radial velocity amplitudes and phases measured for individual spectral lines as tools for a 3D tomography of the atmosphere of HD 24712.
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 stars: atmospheres
653 a stars: chemically peculiar
653 a stars: individual: HD 24712
653 a stars: magnetic fields
653 a stars: oscillations
653 a Astronomy and astrophysics
653 a Astronomi och astrofysik
7001 a Sachkov, M.4 aut
7001 a Weiss, W.W.4 aut
7001 a Kallinger, T.4 aut
7001 a Kochukhov, Olegu Uppsala universitet,Institutionen för astronomi och rymdfysik4 aut0 (Swepub:uu)oko28508
7001 a Bagnulo, S.4 aut
7001 a Ilyin, I.4 aut
7001 a Landstreet, J.D.4 aut
7001 a Leone, F.4 aut
7001 a Lo Curto, G.u Uppsala universitet,Institutionen för astronomi och rymdfysik4 aut
7001 a Luftinger, T.4 aut
7001 a Lyashko, D.4 aut
7001 a Magazzu, A.4 aut
7102 a Uppsala universitetb Institutionen för astronomi och rymdfysik4 org
7730 t Astronomy and Astrophysicsd : EDP Sciencesg 462:3, s. 1103-1112q 462:3<1103-1112x 0004-6361x 1432-0746
8564 u https://www.aanda.org/articles/aa/pdf/2007/06/aa6365-06.pdf
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-14075
8564 8u https://doi.org/10.1051/0004-6361:20066365

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