Photometric classification of the O-B stars

Bigay, J. H.; Garnier, R.

doi:10.1016/0083-6656(74)90008-7

Cited by 2 publications

(2 citation statements)

References 8 publications

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“…Since HAEBE objects are often variable at near-IR wavelengths (e.g., Skrutskie et al 1996), we obtained nearly contemporaneous photometric K-band measurements for our sample, as described in §2.1. As in ELAHS, we calculate F * and F x using our K-band photometry (Table 1) combined with BVRI photometry, visual extinctions, stellar radii, and effective temperatures from the literature (Herbst & Shevchenko 1999;Hillenbrand et al 1992;Oudmaijer et al 2001;de Winter et al 2001;Eiroa et al 2002;Vieira et al 2003;Bigay & Garnier 1970) For several sources where literature values were not available, we computed the stellar parameters using the published spectral types and photometry. The spectral type gives the effective temperature and expected color, from which we determine the extinction.…”

Section: Stellar Emissionmentioning

confidence: 99%

Resolved Inner Disks around Herbig Ae/Be Stars

Eisner

Lane

Hillenbrand

et al. 2004

ApJ

190

304

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We have observed 14 Herbig Ae/Be sources with the long-baseline near-IR Palomar Testbed Interferometer, All except two sources are resolved at 2.2 um, with angular sizes generally <5 mas. We determine the size scales and orientations of the 2.2 um emission using various models: uniform disks, Gaussians, uniform rings, flat accretion disks with inner holes, and flared disks with puffed-up inner rims; 7 objects display significantly inclined morphologies, generally compatible with the outer disk geometries inferred from millimeter interferometric observations, implying that HAEBE disks are not significantly warped. Using the derived inner disk sizes and inclinations, we compute the spectral energy distributions for two simple physical disk models, and compare these with observed SEDs compiled from the literature and new near-IR photometry. While geometrically flat accretion disk models are consistent with the data for the earliest spectral types in our sample (MWC 297, V1685 Cyg, and MWC 1080), the later-type sources are explained better through models incorporating puffed-up inner disk walls; this may indicate different accretion mechanisms for early and late-type Herbig Ae/Be stars.Comment: 54 pages, including 16 figures. Accepted for publication in the Astrophysical Journal (October 2004 issue

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Section: Stellar Emissionmentioning

confidence: 99%

Resolved Inner Disks around Herbig Ae/Be Stars

Eisner

Lane

Hillenbrand

et al. 2004

ApJ

190

304

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“…Following HSVK and MST, we calculate F * and F x using our K-band photometry (Table 1) combined with BVRI photometry, visual extinctions, and stellar effective temperatures from the literature (HSVK; Oudmaijer et al 2001;Eiroa et al 2001;Bigay & Garnier 1970). De-reddening uses the extinction law of Steenman & Thé (1991).…”

Section: Photometrymentioning

confidence: 99%

Near‐Infrared Interferometric Measurements of Herbig Ae/Be Stars

Eisner

Lane

Akeson

et al. 2003

ApJ

116

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We have observed the Herbig Ae/Be sources AB Aur, VV Ser, V1685 Cyg (BD +40 4124), AS 442, and MWC 1080 with the Palomar Testbed Interferometer, obtaining the longest baseline near-IR interferometric observations of this class of objects. All of the sources are resolved at 2.2 lm with angular size scales generally d5 mas, consistent with the only previous near-IR interferometric measurements of Herbig Ae/Be stars, by Millan-Gabet and collaborators. We determine the angular size scales and orientations predicted by uniform-disk, Gaussian, ring, and accretion disk models. Although it is difficult to distinguish different radial distributions, we are able to place firm constraints on the inclinations of these models, and our measurements are the first that show evidence for significantly inclined morphologies. In addition, the derived angular sizes for the early-type Herbig Be stars in our sample, V1685 Cyg and MWC 1080, agree reasonably well with those predicted by the face-on accretion disk models used by Hillenbrand and collaborators to explain observed spectral energy distributions. In contrast, our data for the later-type sources AB Aur, VV Ser, and AS 442 are somewhat inconsistent with these models and may be explained better through the puffed-up inner disk models of Dullemond and collaborators.

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Photometric classification of the O-B stars

Cited by 2 publications

References 8 publications

Resolved Inner Disks around Herbig Ae/Be Stars

Resolved Inner Disks around Herbig Ae/Be Stars

Near‐Infrared Interferometric Measurements of Herbig Ae/Be Stars

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