Bright Blazhko RRab Lyrae stars observed by ASAS and the
SuperWASP surveys

J 2014

Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys

SKARKA, Marek

Basic information

Original name

Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys

Authors

SKARKA, Marek (203 Czech Republic, guarantor, belonging to the institution)

Edition

Astronomy and Astrophysics, 2014, 0004-6361

Other information

Language

English

Type of outcome

Article in a journal

Field of Study

10308 Astronomy

Country of publisher

France

Confidentiality degree

is not subject to a state or trade secret

References:

URL

Impact factor

Impact factor: 4.378

RIV identification code

RIV/00216224:14310/14:00075061

Organization unit

Faculty of Science

DOI

https://doi.org/10.1051/0004-6361/201322491

UT WoS

000332161800076

EID Scopus

2-s2.0-84894354802

Keywords in English

Astronomical data bases: miscellaneous – Stars: horizontal-branch – Stars: variables: RR Lyr – Stars: individual: IK Hya

Abstract

In the original language

Period study of 321 fundamental mode galactic field RR Lyrae type stars (RRab), which had appropriate data in ASAS and SuperWASP surveys, brighter than 12.5 mag in maximum light was performed. We found 100 stars to be definitely modulated. In 25 cases, previously unknown modulation was revealed and 8 new candidates for Blazhko stars were identified. In 18 previously found Blazhko stars, no modulation was detectable. Multiple modulation was revealed for eight stars that were previously proposed to show simple modulation. In total, there were twelve stars with some peculiarity in their modulation in the sample. This brings the incidence rate of multiple/irregularly-modulated stars to 12 %. The ratio of the modulation periods of five of the double-modulated stars was within the ratios of small integers. One of stars studied, IK Hya, showed a very interesting frequency spectrum, which we interpret as changing Blazhko period between 71.81 and 75.57 days and an additional 1403-day-long cycle analogous to a four-year cycle of the prototype RR Lyr. The limits of the shorter period produce a beating period that is approximately twice as big as a 1403-day period. The newly revealed Blazhko star RZ CVn seems to undergo changes in the amplitude of the modulation, as well as in the basic pulsation and Blazhko periods. We found that the incidence rate of the Blazhko RR Lyraes is at least 31 %, more likely even higher. It was also found that the majority of the Blazhko variables show triplet structures in their frequency spectra and that in 89 % of these cases, the peak with larger amplitude is on the right-hand side of the main pulsation component.

Links

MUNI/A/0735/2012, interní kód MU

Name: Fyzika hvězd a vesmíru

Investor: Masaryk University, Category A

MUNI/A/0968/2009, interní kód MU

Name: Fyzika hvězd a hvězdných soustav (Acronym: FYHA)

Investor: Masaryk University, Category A

Cite

SKARKA, Marek. Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys. Astronomy and Astrophysics. 2014, vol. 562, february, p. "nestrankovano", 14 pp. ISSN 0004-6361. Available from: https://doi.org/10.1051/0004-6361/201322491.

@article{1166200,
   author = {Skarka, Marek},
   article_number = {february},
   doi = {https://doi.org/10.1051/0004-6361/201322491},
   keywords = {Astronomical data bases: miscellaneous – Stars: horizontal-branch – Stars: variables: RR Lyr – Stars: individual: IK Hya},
   language = {eng},
   issn = {0004-6361},
   journal = {Astronomy and Astrophysics},
   title = {Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys},
   url = {http://adsabs.harvard.edu/abs/2014A%26A...562A..90S},
   volume = {562},
   year = {2014}
}

TY  - JOUR
ID  - 1166200
AU  - Skarka, Marek
PY  - 2014
TI  - Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys
JF  - Astronomy and Astrophysics
VL  - 562
IS  - february
SP  - "nestrankovano"
EP  - "nestrankovano"
SN  - 00046361
KW  - Astronomical data bases: miscellaneous – Stars: horizontal-branch – Stars: variables: RR Lyr – Stars: individual: IK Hya
UR  - http://adsabs.harvard.edu/abs/2014A%26A...562A..90S
L2  - http://adsabs.harvard.edu/abs/2014A%26A...562A..90S
N2  - Period study of 321 fundamental mode galactic field RR Lyrae type stars (RRab), which had appropriate data in ASAS and SuperWASP surveys, brighter than 12.5 mag in maximum light was performed. We found 100 stars to be definitely modulated. In 25 cases, previously unknown modulation was revealed and 8 new candidates for Blazhko stars were identified. In 18 previously found Blazhko stars, no modulation was detectable. Multiple modulation was revealed for eight stars that were previously proposed to show simple modulation. In total, there were twelve stars with some peculiarity in their modulation in the sample. This brings the incidence rate of multiple/irregularly-modulated stars to 12 %. The ratio of the modulation periods of five of the double-modulated stars was within the ratios of small integers. One of stars studied, IK Hya, showed a very interesting frequency spectrum, which we interpret as changing Blazhko period between 71.81 and 75.57 days and an additional 1403-day-long cycle analogous to a four-year cycle of the prototype RR Lyr. The limits of the shorter period produce a beating period that is approximately twice as big as a 1403-day period. The newly revealed Blazhko star RZ CVn seems to undergo changes in the amplitude of the modulation, as well as in the basic pulsation and Blazhko periods. We found that the incidence rate of the Blazhko RR Lyraes is at least 31 %, more likely even higher. It was also found that the majority of the Blazhko variables show triplet structures in their frequency spectra and that in 89 % of these cases, the peak with larger amplitude is on the right-hand side of the main pulsation component.
ER  -

SKARKA, Marek. Bright Blazhko RRab Lyrae stars observed by ASAS and the SuperWASP surveys. \textit{Astronomy and Astrophysics}. 2014, vol.~562, february, p.~''nestrankovano'', 14 pp. ISSN~0004-6361. Available from: https://doi.org/10.1051/0004-6361/201322491.

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