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An investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data

The result's identifiers

  • Result code in IS VaVaI

    <a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F18%3A00104476" target="_blank" >RIV/00216224:14310/18:00104476 - isvavai.cz</a>

  • Result on the web

    <a href="http://dx.doi.org/10.1093/mnras/sty1320" target="_blank" >http://dx.doi.org/10.1093/mnras/sty1320</a>

  • DOI - Digital Object Identifier

    <a href="http://dx.doi.org/10.1093/mnras/sty1320" target="_blank" >10.1093/mnras/sty1320</a>

Alternative languages

  • Result language

    angličtina

  • Original language name

    An investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data

  • Original language description

    We present an investigation of a large sample of confirmed (N = 233) and candidate (N = 54) Galactic classical Be stars (mean V magnitude range of 6.4-12.6 mag), with the main aim of characterizing their photometric variability. Our sample stars were preselected among early-type variables using light-curve morphology criteria. Spectroscopic information was gleaned from the literature, and archival and newly acquired spectra. Photometric variability was analysed using archival ASAS-3 time-series data. To enable a comparison of results, we have largely adopted the methodology of Labadie-Bartz et al. (2017), who carried out a similar investigation based on KELT data. Complex photometric variations were established in most stars: outbursts on different time-scales (in 73 +/- 5 per cent of stars), long-term variations (36 +/- 6 per cent), periodic variations on intermediate time-scales (1 +/- 1 per cent), and short-term periodic variations (6 +/- 3 per cent). 24 +/- 6 per cent of the outbursting stars exhibit (semi) periodic outbursts. We close the apparent void of rare outbursters reported by Labadie-Bartz et al. (2017) and show that Be stars with infrequent outbursts are not rare. While we do not find a significant difference in the percentage of stars showing outbursts among early-type, mid-type, and late-type Be stars, we show that early-type Be stars exhibit much more frequent outbursts. We have measured rising and falling times for well-covered and well-defined outbursts. Nearly all outburst events are characterized by falling times that exceed the rising times. No differences were found between early-, mid-, and late-type stars; a single non-linear function adequately describes the ratio of falling time to rising time across all spectral subtypes, with the ratio being larger for short events.

  • Czech name

  • Czech description

Classification

  • Type

    J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database

  • CEP classification

  • OECD FORD branch

    10308 - Astronomy (including astrophysics,space science)

Result continuities

  • Project

    <a href="/en/project/7AMB17AT030" target="_blank" >7AMB17AT030: The analysis of spotted stars using high precision data</a><br>

  • Continuities

    P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)<br>S - Specificky vyzkum na vysokych skolach<br>I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Others

  • Publication year

    2018

  • Confidentiality

    S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Data specific for result type

  • Name of the periodical

    Monthly Notices of the Royal Astronomical Society

  • ISSN

    0035-8711

  • e-ISSN

  • Volume of the periodical

    479

  • Issue of the periodical within the volume

    3

  • Country of publishing house

    GB - UNITED KINGDOM

  • Number of pages

    59

  • Pages from-to

    2909-2967

  • UT code for WoS article

    000441382300005

  • EID of the result in the Scopus database

    2-s2.0-85051533134