Spectral Analysis and Classification of Herbig Ae/Be Stars

By Jesús Hernández, N. Calvet, C. Briceño, L. Hartmann, P. Berlind. 2004

243 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/07fb97f0ea7be70d3b49b6c850356e7a8400cdf3

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Citations in the corpus

Herbig Ae/Be Stars in nearby OB Associations (2004, methodology): “The Herbig Ae/Be (HAeBe) stars are young emission-line objects with spectral types B, A, and in a few cases F, in most instances spatially correlated with dark clouds or bright nebulosities (Herbig 1960; Waters & Waelkens 1998; Hernández et al. 2004).”
KINEMATIC AND SPATIAL SUBSTRUCTURE IN NGC 2264 (2015, methodology): “We used SPTCLASS, a semi-automatic spectraltyping program (Hernández et al. 2004), which uses empirical relations of spectral type and absorption line equivalent widths for classification (see Hsu et al. 2012 for details).”
UNVEILING THE STRUCTURE OF PRE-TRANSITIONAL DISKS (2010, methodology): “Spectral Type Classification Spectral types were derived with the SPTCLASS tool,12 an IRAF/IDL code based on the methods described by Hernández et al. (2004).”
AN OPTICAL SPECTROSCOPIC STUDY OF T TAURI STARS. I. PHOTOSPHERIC PROPERTIES (2014, background): “While RY Tau has had numerous spectral types bewteen F7–G1 Mora et al. (2001); Calvet et al. (2004); Hernandez et al. (2004), the Cohen & Kuhi (1979) spectral type of K1 has been adopted in several recent compulations.”
Circumstellar Dust Disks in Taurus-Auriga: The Submillimeter Perspective (2005, background): “Our sample was selected primarily from the compilation of Kenyon & Hartmann (1995), and was designed to contain roughly equal numbers of Class II and III objects, WTTSs and CTTSs, and single and multiple stars.”
C2D Spitzer-IRS spectra of disks around T Tauri stars. II. PAH emission features (2006, unknown): “…Acke & van den Ancker (2004), 9: Dunkin et al. (1997), 10: Acke et al. (2005), 11: Assumed distance to Taurus-Auriga cloud (Kenyon et al. 1994), 12: Hernández et al. (2004), 13: Mora et al. (2001), 14: Straizys et al. (1996), 15: Finkenzeller & Mundt (1984), 16: Thé et al. (1994), 17: Houk…”
A high-resolution spectropolarimetric survey of Herbig Ae/Be stars – I. Observations and measurements (2012, methodology): “…et al. (1996); (al) van Leeuwen (2007); (am) Vieira et al. (2003); (an) Wolff et al. (2004); (ao) Folsom et al. (2012); (ap) Montesinos et al. (2009); (aq) Hernández et al. (2004); (ar) Mora et al. (2004); (as) Fossati et al. (2009); (at) Miroshnichenko et al. (2004); (au) Hernández et al.…”
[O I] 6300 Å emission in Herbig Ae/Be systems: Signature of Keplerian rotation (2005, background): “The forbidden oxygen 6300Å emission line in Herbig Ae/B stars has been studied in previous articles (Finkenzeller 1985; Böhm & Catala 1994; Hamann 1994; Böhm & Hirth 1997; Corcoran & Ray 1997, 1998; Hernández et al. 2004).”
A spectroscopic survey of Herbig Ae/Be stars with X-shooter – I. Stellar parameters and accretion rates (2015, methodology): “It is possible that the total-toselective extinction may be higher, possibly RV = 5.0, for some of the stars in this sample based on previous analysis of HAeBes (Hernández et al. 2004; Manoj et al. 2006).”
Sub-arcsec imaging of the AB Aur molecular disk and envelope at millimeter wavelengths: a non Keplerian disk (2005, methodology): “It has a spectral type A0-A1 (Hernández et al. 2004) and is located at a distanceD = 144±2317 pc following Send offprint requests to: S.Guilloteau, e-mail: guilloteau@obs.u-bordeaux1.fr ⋆ Based on observations carried out with the IRAM Plateau de Bur Interferometer.”
Magnetospheres and Disk Accretion in Herbig Ae/Be Stars (2004, methodology): “…of UX Ori, discussed in x 2, the optical spectrum shows that only H is in emission, and there is no veiling in the absorption lines; analysis of the spectra as in Hernández et al. (2004) yields a spectral type of A2 1 subclass, using as indicators the Ca ii K line, Fe ii lines, Ca i lines, and H .”
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, unknown): “…is ±1 subclass. bThe spectral classifications were collated from the following references: 1 = Luhman et al. (2010), 2 = Hartigan & Kenyon (2003), 3 = Hernández et al. (2004), 4 = Furlan et al. (2011), 5 = White & Ghez (2001), 6 = Itoh et al. (2005), 7 = Espaillat et al. (2010), 8 =…”
Star and Protoplanetary Disk Properties in Orion's Suburbs (2009, methodology): “We determined the spectral types of the stars for which we hav VIMOS spectroscopy using the classification scheme developed by Hernández et al. (2004).”
Accretion disks in luminous young stellar objects (2015, background): “This can lead to uncertainties in spectral type of 5 sub-types and in some cases it can be even more uncertain (Hernandez et al., 2004; Alecian et al., 2013).”
A Spitzer Space Telescope Study of Disks in the Young σ Orionis Cluster (2007, background): “This object alternatively could be considered to be an IMTTS, as F5 is the usual transition spectral type between HAeBe stars and IMTTSs (see Hernández et al. 2004).”