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PRVÁK, Milan, Jiří LIŠKA, Jiří KRTIČKA, Zdeněk MIKULÁŠEK a Theresa LUFTINGER. Modelling of variability of the chemically peculiar star phi Draconis. ASTRONOMY & ASTROPHYSICS. LES ULIS CEDEX A: EDP SCIENCES S A, 2015, roč. 584, December, s. "nestránkováno", 9 s. ISSN 1432-0746. Dostupné z: https://dx.doi.org/10.1051/0004-6361/201526647.

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TY  - JOUR
ID  - 1338859
AU  - Prvák, Milan - Liška, Jiří - Krtička, Jiří - Mikulášek, Zdeněk - Luftinger, Theresa
PY  - 2015
TI  - Modelling of variability of the chemically peculiar star phi Draconis
JF  - ASTRONOMY & ASTROPHYSICS
VL  - 584
IS  - December
SP  - "nestránkováno"
EP  - "nestránkováno"
PB  - EDP SCIENCES S A
SN  - 14320746
KW  - stars: chemically peculiar
KW  - stars: early-type
KW  - stars: variables: general
KW  - stars: individual: phi Dra
N2  - Context. The presence of heavier chemical elements in stellar atmospheres influences the spectral energy distribution of stars. An uneven surface distribution of these elements, together with flux redistribution and stellar rotation, are commonly believed to be the primary causes of the variability of chemically peculiar (CP) stars. Aims. We aim to model the photometric variability of the CP star. Dra based on the assumption of inhomogeneous surface distribution of heavier elements and compare it to the observed variability of the star. We also intend to identify the processes that contribute most significantly to its photometric variability. Methods. We use a grid of TLUSTY model atmospheres and the SYNSPEC code to model the radiative flux emerging from the individual surface elements of. Dra with different chemical compositions. We integrate the emerging flux over the visible surface of the star at different phases throughout the entire rotational period to synthesise theoretical light curves of the star in several spectral bands. Results. The synthetic light curves in the visible and in the near-UV regions are in very good agreement with the observed variability of the star. The lack of usable far-UV measurements of the star precludes making any conclusions about the correctness of our model in this spectral region. We also obtained 194 new BVRI observations of phi Dra and improved its rotational period to P = 1.(d)716500(2). Conclusions. We show that the inhomogeneous distribution of elements, flux redistribution, and rotation of the star are fully capable of explaining the stellar variability in the visible and the near-UV regions. The flux redistribution is mainly caused by bound-free transitions of silicon and bound-bound transitions of iron.
ER  -

Základní údaje
Originální název	Modelling of variability of the chemically peculiar star phi Draconis
Název česky	Modelování proměnnosti chemicky pekuliární hvězdy fí Draconis
Autoři	PRVÁK, Milan (203 Česká republika, garant, domácí), Jiří LIŠKA (203 Česká republika, domácí), Jiří KRTIČKA (203 Česká republika, domácí), Zdeněk MIKULÁŠEK (203 Česká republika, domácí) a Theresa LUFTINGER (40 Rakousko).
Vydání	ASTRONOMY & ASTROPHYSICS, LES ULIS CEDEX A, EDP SCIENCES S A, 2015, 1432-0746.

Další údaje
Originální jazyk	angličtina
Typ výsledku	Článek v odborném periodiku
Obor	10308 Astronomy
Stát vydavatele	Francie
Utajení	není předmětem státního či obchodního tajemství
Impakt faktor	Impact factor: 5.185
Kód RIV	RIV/00216224:14310/15:00081639
Organizační jednotka	Přírodovědecká fakulta
Doi	http://dx.doi.org/10.1051/0004-6361/201526647
UT WoS	000366936800017
Klíčová slova anglicky	stars: chemically peculiar; stars: early-type; stars: variables: general; stars: individual: phi Dra
Štítky	AKR, rivok
Příznaky	Mezinárodní význam, Recenzováno
Změnil	Změnila: Ing. Andrea Mikešková, učo 137293. Změněno: 7. 4. 2016 10:38.

Anotace
Context. The presence of heavier chemical elements in stellar atmospheres influences the spectral energy distribution of stars. An uneven surface distribution of these elements, together with flux redistribution and stellar rotation, are commonly believed to be the primary causes of the variability of chemically peculiar (CP) stars. Aims. We aim to model the photometric variability of the CP star. Dra based on the assumption of inhomogeneous surface distribution of heavier elements and compare it to the observed variability of the star. We also intend to identify the processes that contribute most significantly to its photometric variability. Methods. We use a grid of TLUSTY model atmospheres and the SYNSPEC code to model the radiative flux emerging from the individual surface elements of. Dra with different chemical compositions. We integrate the emerging flux over the visible surface of the star at different phases throughout the entire rotational period to synthesise theoretical light curves of the star in several spectral bands. Results. The synthetic light curves in the visible and in the near-UV regions are in very good agreement with the observed variability of the star. The lack of usable far-UV measurements of the star precludes making any conclusions about the correctness of our model in this spectral region. We also obtained 194 new BVRI observations of phi Dra and improved its rotational period to P = 1.(d)716500(2). Conclusions. We show that the inhomogeneous distribution of elements, flux redistribution, and rotation of the star are fully capable of explaining the stellar variability in the visible and the near-UV regions. The flux redistribution is mainly caused by bound-free transitions of silicon and bound-bound transitions of iron.

Anotace

Context. The presence of heavier chemical elements in stellar atmospheres influences the spectral energy distribution of stars. An uneven surface distribution of these elements, together with flux redistribution and stellar rotation, are commonly believed to be the primary causes of the variability of chemically peculiar (CP) stars. Aims. We aim to model the photometric variability of the CP star. Dra based on the assumption of inhomogeneous surface distribution of heavier elements and compare it to the observed variability of the star. We also intend to identify the processes that contribute most significantly to its photometric variability. Methods. We use a grid of TLUSTY model atmospheres and the SYNSPEC code to model the radiative flux emerging from the individual surface elements of. Dra with different chemical compositions. We integrate the emerging flux over the visible surface of the star at different phases throughout the entire rotational period to synthesise theoretical light curves of the star in several spectral bands. Results. The synthetic light curves in the visible and in the near-UV regions are in very good agreement with the observed variability of the star. The lack of usable far-UV measurements of the star precludes making any conclusions about the correctness of our model in this spectral region. We also obtained 194 new BVRI observations of phi Dra and improved its rotational period to P = 1.(d)716500(2). Conclusions. We show that the inhomogeneous distribution of elements, flux redistribution, and rotation of the star are fully capable of explaining the stellar variability in the visible and the near-UV regions. The flux redistribution is mainly caused by bound-free transitions of silicon and bound-bound transitions of iron.

Návaznosti
GAP209/12/0217, projekt VaV	Název: Multispektrální proměnnost horkých hvězd a její příčiny
GAP209/12/0217, projekt VaV	Investor: Grantová agentura ČR, Multispektrální proměnnost horkých hvězd a její příčiny
GA13-10589S, projekt VaV	Název: Ztráta hmoty horkých hmotných hvězd
GA13-10589S, projekt VaV	Investor: Grantová agentura ČR, Ztráta hmoty horkých hmotných hvězd