Modelling of variability of the chemically peculiar star phi
Draconis

J 2015

Modelling of variability of the chemically peculiar star phi Draconis

PRVÁK, Milan, Jiří LIŠKA, Jiří KRTIČKA, Zdeněk MIKULÁŠEK, Theresa LUFTINGER et. al.

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

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

Změněno: 7. 4. 2016 10:38, Ing. Andrea Mikešková

Anotace

V originále

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

Investor: Grantová agentura ČR, Multispektrální proměnnost horkých hvězd a její příčiny

GA13-10589S, projekt VaV

Název: Ztráta hmoty horkých hmotných hvězd

Investor: Grantová agentura ČR, Ztráta hmoty horkých hmotných hvězd

Citovat

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.

@article{1338859,
   author = {Prvák, Milan and Liška, Jiří and Krtička, Jiří and Mikulášek, Zdeněk and Luftinger, Theresa},
   article_location = {LES ULIS CEDEX A},
   article_number = {December},
   doi = {http://dx.doi.org/10.1051/0004-6361/201526647},
   keywords = {stars: chemically peculiar; stars: early-type; stars: variables: general; stars: individual: phi Dra},
   language = {eng},
   issn = {1432-0746},
   journal = {ASTRONOMY & ASTROPHYSICS},
   title = {Modelling of variability of the chemically peculiar star phi Draconis},
   volume = {584},
   year = {2015}
}

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  -

PRVÁK, Milan, Jiří LIŠKA, Jiří KRTIČKA, Zdeněk MIKULÁŠEK a Theresa LUFTINGER. Modelling of variability of the chemically peculiar star phi Draconis. \textit{ASTRONOMY \&{}amp; 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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