An infrared study of Herbig Ae/Be stars

Zhang, P.; Yang, Haifeng; Liu, J.

doi:10.1007/s10509-005-9031-6

Cited by 9 publications

(7 citation statements)

References 30 publications

(30 reference statements)

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“…We have gathered the majority of Herbig Ae/Be stars known and proposed to date from different works (272, see Chen et al 2016 for a compilation of most of them). Chen et al (2016) based their sample mostly on the work of Zhang et al (2006) which in turn is based on the work of The et al (1994) and Vieira et al (2003). In addition, we included a few HAeBes from ; Baines et al (2006); Carmona et al 2010;Hernández et al (2005); Manoj et al (2006) and Sartori et al (2010) that are not present in the aforementioned papers.…”

Section: Construction Of the Samplementioning

confidence: 99%

GaiaDR2 study of Herbig Ae/Be stars

Vioque

Oudmaijer

Baines

et al. 2018

A&A

174

313

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Aims. We use Gaia Data Release 2 (DR2) to place 252 Herbig Ae/Be stars in the HR diagram and investigate their characteristics and properties. Methods. For all known Herbig Ae/Be stars with parallaxes in Gaia DR2, we collected their atmospheric parameters and photometric and extinction values from the literature. To these data we added near-and mid-infrared photometry, collected Hα emission line properties such as equivalent widths and line profiles, and their binarity status. In addition, we developed a photometric variability indicator from Gaia's DR2 information.Results. We provide masses, ages, luminosities, distances, photometric variabilities and infrared excesses homogeneously derived for the most complete sample of Herbig Ae/Be stars to date. We find that high mass stars have a much smaller infrared excess and have much lower optical variabilities compared to lower mass stars, with the break at around 7M . Hα emission is generally correlated with infrared excess, with the correlation being stronger for infrared emission at wavelengths tracing the hot dust closest to the star. The variability indicator as developed by us shows that ∼25% of all Herbig Ae/Be stars are strongly variable. We observe that the strongly variable objects display doubly peaked Hα line profiles, indicating an edge-on disk.Conclusions. The fraction of strongly variable Herbig Ae stars is close to that found for A-type UX Ori stars. It had been suggested that this variability is in most cases due to asymmetric dusty disk structures seen edge-on. The observation here is in strong support of this hypothesis. Finally, the difference in dust properties occurs at 7M , while various properties traced at UV/optical wavelengths differ at a lower mass, 3M . The latter has been linked to different accretion mechanisms at work whereas the differing infrared properties and photometric variabilities are related to different or differently acting (dust-)disk dispersal mechanisms.

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Section: Construction Of the Samplementioning

confidence: 99%

GaiaDR2 study of Herbig Ae/Be stars

Vioque

Oudmaijer

Baines

et al. 2018

A&A

174

313

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“…It is notable that there are three stars (out of these 10 Be stars with ISO SWS01 spectra) that also appear in the Herbig Ae/Be members and candidate members listed by some authors (e.g. Thé et al 1994;Vieira et al 2003;Zhang et al 2006). Because it is very difficult to determine whether these stars are really Be stars or Herbig Be stars, we will study them as Be stars in this paper.…”

Section: Sample Datamentioning

confidence: 93%

An infrared study of Be stars based on ISO SWS01 spectra

Zhang

2009

Res. Astron. Astrophys.

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The Infrared Space Observatory (ISO) Short-Wavelength Spectrometer (SWS) spectra of 10 Be stars are presented. It can be seen that the Be stars show a diversity in their ISO SWS01 spectral classifications by Kraemer et al., from naked stars, stars associated with dust, stars with warm dust shells, stars with cool dust shells to very red sources. In addition, the Brα/HI(14-6) line flux ratio derived for the sample stars is compared with that of P Cyg, and it is found that the line ratio of Be stars which were investigated show not only lower values as suggested by Waters et al., but also larger values. Therefore, the line ratio cannot be used to judge whether a star is a Be star or not.

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“…Subsequently, Strom et al (1972) extended the HAeBes definition with additional properties, including infrared (IR) excess, time variation, linear polarization, and association with starforming regions. Since then, the HAeBes data set has been enlarged by numerous studies over decades (Finkenzeller & Mundt 1984;The et al 1994;Vieira et al 2003;Hernández et al 2005;Zhang et al 2006;Manoj et al 2006;Baines et al 2006;Sartori et al 2010;Carmona et al 2010;Alecian et al 2013;Fairlamb et al 2015;Chen et al 2016;Vioque et al 2018;Keller et al 2019;Moura et al 2020;Vioque et al 2020;Pereira et al 2021;Zhang et al 2022;Vioque et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Identification and parameter determination of F-type Herbig stars from LAMOST DR8

Zhang¹,

Luo²,

Jiang³

et al. 2022

Preprint

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We identify 20 F-type Herbig stars and provide a list of 22 pre-main-sequence candidates from LAMOST DR8. The effective temperature, distance, extinction, stellar luminosity, mass, and radius are derived for each Herbig star based on optical spectra, photometry, Gaia EDR3 parallaxes, and pre-main-sequence evolutionary tracks. According to spectral energy distributions, 19 F-type Herbig stars belong to Class II YSOs, and one belongs to the flat-spectrum class. Four have Spitzer IRS spectra, of which three show extremely weak polycyclic aromatic hydrocarbons emissions, and three with both amorphous and crystalline silicate emissions share the similar parameters and are at the same evolutionary stage. We detect a solar-nearby outbursting EXor Herbig star J034344.48+314309.3, possible precursor of a Herbig Ae star. Intense emission lines of HI, HeI, OI, NaI, and CaII originated from the rapid accretion during the outbursts are detected in its optical spectra, and silicate emission features are detected in its infrared spectrum. We also make a statistic analysis on the disk properties of all known Herbig stars using the defined infrared spectral indices (α J−K S and α K S −W 3 ). The proportion of Herbig stars with moderate infrared excesses decreases as effective temperature increases. The majority of the precursors (F-, G-, or K-type) have moderate infrared excesses. Hotter Herbig stars tend to have a larger proportion with large infrared excesses. The trends may be due to the fact that hotter stars have larger areas of re-emitting dust, although there is some scatter due to the particularities of each disk.

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An infrared study of Herbig Ae/Be stars

Cited by 9 publications

References 30 publications

GaiaDR2 study of Herbig Ae/Be stars

GaiaDR2 study of Herbig Ae/Be stars

An infrared study of Be stars based on ISO SWS01 spectra

Identification and parameter determination of F-type Herbig stars from LAMOST DR8

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