2011A&A...527A.103W


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST07:15:25

2011A&A...527A.103W - Astronomy and Astrophysics, volume 527A, 103-103 (2011/3-1)

VLTI/AMBER spectro-interferometry of the Herbig Be star MWC 297 with spectral resolution 12000.

WEIGELT G., GRININ V.P., GROH J.H., HOFMANN K.-H., KRAUS S., MIROSHNICHENKO A.S., SCHERTL D., TAMBOVTSEVA L.V., BENISTY M., DRIEBE T., LAGARDE S., MALBET F., MEILLAND A., PETROV R. and TATULLI E.

Abstract (from CDS):

Circumstellar disks and outflows play a fundamental role in star formation. Infrared spectro-interferometry allows the inner accretion-ejection region to be resolved. We study the disk and Brγ-emitting region of MWC 297 with high spatial and spectral resolution and compare our observations with disk-wind models. We measured interferometric visibilities, wavelength-differential phases, and closure phases of MWC 297 with a spectral resolution of 12000. To interpret our MWC 297 observations, we employed disk-wind models. The measured continuum visibilities confirm previous results that the continuum-emitting region of MWC 297 is remarkably compact. We derive a continuum ring-fit radius of ∼2.2mas (∼0.56AU at a distance of 250pc), which is ∼5.4 times smaller than the 3 AU dust sublimation radius expected for silicate grains (in the absence of radiation-shielding material). The strongly wavelength-dependent and asymmetric Brγ-emitting region is more extended (∼2.7times) than the continuum-emitting region. At the center of the Brγ line, we derive a Gaussian fit radius of ∼6.3mas HWHM (∼1.6AU). To interpret the observations, we employ a magneto-centrifugally driven disk-wind model consisting of an accretion disk, which emits the observed continuum radiation, and a disk wind, which emits the Brγ line. The calculated wavelength-dependent model intensity distributions and Brγ line profiles are compared with the observations (i.e., K-band spectrum, visibilities, differential phases, and closure phases). The closest fitting model predicts a continuum-emitting disk with an inner radius of ∼0.3AU and a disk wind ejection region with an inner radius of ∼0.5AU (∼17.5 stellar radii). We obtain a disk-wind half-opening angle (the angle between the rotation axis and the innermost streamline of the disk wind) of ∼80°, which is larger than in T Tau models, and a disk inclination angle of ∼20° (i.e., almost pole-on). Our observations with a spectral resolution of 12000 allow us to study the AU-scale environment of MWC 297 in ∼10 different spectral channels across the Brγ emission line. We show that the K-band flux, visibilities, and remarkably strong phases can be explained by the employed magneto-centrifugally driven disk wind model.

Abstract Copyright:

Journal keyword(s): stars: individual: MWC 297 - stars: pre-main sequence - stars: winds, outflows - circumstellar matter - techniques: interferometric - techniques: spectroscopic

Simbad objects: 3

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Number of rows : 3

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 803 0
2 EM* MWC 297 Ae* 18 27 39.5266257570 -03 49 52.136526892 15.57 14.34 12.31 11.34   B1.5Ve 266 0
3 HD 175583 * 18 56 44.4799307033 -17 26 38.762971327   8.59 7.08     K2III 9 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-07:15:25

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