MIKULÁŠEK, Zdeněk, Jiří KRTIČKA, G.W. HENRY, Jan JANÍK, Miloslav ZEJDA, T. LUEFTINGER, Ernst PAUNZEN, I. I. ROMANYUK and D.O. KUDRYAVTSEV. Rotational period variations in magnetic chemically peculiar star HD 37776. In European Week of Astronomy and Space Science, JENAM 2011, July 4 to 8 2011 in Saint-Petersburg, Russia. 2011.
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Basic information
Original name Rotational period variations in magnetic chemically peculiar star HD 37776
Authors MIKULÁŠEK, Zdeněk (203 Czech Republic, guarantor, belonging to the institution), Jiří KRTIČKA (203 Czech Republic, belonging to the institution), G.W. HENRY (840 United States of America), Jan JANÍK (203 Czech Republic, belonging to the institution), Miloslav ZEJDA (203 Czech Republic, belonging to the institution), T. LUEFTINGER (40 Austria), Ernst PAUNZEN (40 Austria), I. I. ROMANYUK (643 Russian Federation) and D.O. KUDRYAVTSEV (643 Russian Federation).
Edition European Week of Astronomy and Space Science, JENAM 2011, July 4 to 8 2011 in Saint-Petersburg, Russia, 2011.
Other information
Original language English
Type of outcome Presentations at conferences
Field of Study 10308 Astronomy
Country of publisher Russian Federation
Confidentiality degree is not subject to a state or trade secret
WWW webovská stránka akce
RIV identification code RIV/00216224:14310/11:00049549
Organization unit Faculty of Science
Keywords (in Czech) chemicky pekuliární hvězdy; magnetické hvězdy; fotometrie; V901 Ori
Keywords in English chemical peculiar star; magnetic stars; photometry; V901 Ori
Tags International impact
Changed by Changed by: doc. RNDr. Miloslav Zejda, Ph.D., učo 169695. Changed: 8/4/2012 18:39.
Abstract
Three decades of a precise photometric and spectroscopic monitoring of the young hot magnetic chemically peculiar star HD 37776 have revealed its continual rotational deceleration, increasing the period by a remarkable 18 s! The deceleration was interpreted as the rotational braking of the outer stellar layers due to the angular momentum loss in the stellar magnetosphere. Observational data have been recently supplemented by own new photometric data. We present here the results of the sophisticated analysis of all available observed data showing that the period reached its maximum of 1.538766 d in the year 2004, when the rotation period began to decrease. The nature of such unpredicted period changes and the paradox of the spin-down time are briefly discussed.
Links
IAA301630901, research and development projectName: Rozložení energie ve spektru horkých hvězd a jeho proměnnost
Investor: Academy of Sciences of the Czech Republic, Spectral energy distribution of hot stars and its variability
MUNI/A/0968/2009, interní kód MUName: Fyzika hvězd a hvězdných soustav (Acronym: FYHA)
Investor: Masaryk University, Category A
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