Integral spectroscopy of the nebula GM 1-29 and the star PV Cep

Movsessian, T. A.; Magakian, T. Yu.; Sargsyan, D. M.; Nikogossian, E. H.

doi:10.1007/s10511-008-9024-6

Cited by 5 publications

(5 citation statements)

References 12 publications

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“…All kinds of shapes from the classification by Reipurth et al are observed: P Cygni, single-and doublepeaked (see, e.g., Böhm & Catala 1995;Grinin et al 2001;Mora et al 2001;Feigelson et al 2003;Beskrovnaya & Pogodin 2004;Movsessian et al 2008;Grady et al 2011;Montesinos 2009;Mendigutía 2012). Such a vast sample of profile shapes suggests that this line originates in a very complex environment possibly including the accretion disk, disk wind, jet, and magnetosphere.…”

Section: Hybrid Model: Disk Wind X-wind and Magnetospherementioning

confidence: 93%

Hydrogen lines as a diagnostic tool for studying multicomponent emitting regions in hot young stars: magnetosphere, X-wind, and disk wind

Тамбовцева

Гринин

Weigelt

2014

A&A

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Infrared interferometric observations with high spatial and spectral resolution and their quantitative modeling provide us with a unique opportunity to improve our understanding of the circumstellar environment of young stars and the accretion-ejection process. The goal of this paper is to investigate various models of the emitting regions in young Herbig Ae/Be stars that consist of (i) a compact rotating magnetosphere; (ii) an X-wind; and (iii) a disk wind. These models can be used, for example, to quantitatively interpret line profile measurements and infrared interferometric observations with the AMBER instrument of the Very Large Telescope Interferometer (VLTI) in the high spectral resolution mode (R = 12 000). VLTI/AMBER observations allow us to resolve the disk wind region and study the flux contribution of the unresolved magnetosphere and X-wind region to the total line flux. Analyzing the results of our non-LTE calculations, we conclude that the mechanisms of the different broadening of emission lines of different series include (1) the kinematic expansion due to the motion of the outflowing, accelerating gas in the magneto-centrifugal disk wind; (2) the Stark effect; and (3) the rotation of the magnetosphere. We also investigated extinction effects that can influence the shape of the line profiles. We considered the obscuration of the outer disk wind by an opaque dust and gas disk, the obscuration of the disk wind by a flared disk or by dust in the disk wind itself, and absorption of the star and disk continuum radiation in the disk wind along the line of sight. We show that due to extinction effects, the line profiles can change from double-peaked to single-peaked and P Cygni profiles. We studied the contribution of the different components of the stellar environment to different hydrogen emission lines and investigated how this contribution is dependent on the model parameters. The results of this study can be used for the detailed modeling of the emitting regions of individual young stars.

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Section: Hybrid Model: Disk Wind X-wind and Magnetospherementioning

confidence: 93%

Hydrogen lines as a diagnostic tool for studying multicomponent emitting regions in hot young stars: magnetosphere, X-wind, and disk wind

Тамбовцева

Гринин

Weigelt

2014

A&A

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“…This asymmetry is the direct result of the existence of the anisotropic expanding stellar envelope around the central star combined with the geometrically favorable projection of its spectrum on the walls of the cavity in the interstellar dust (we see these walls as the bright conical nebula, which reflect the spectrum of the envelope at various latitudes in the line-of-sight direction). Besides the classic example of R Mon (Jones & Herbig 1982), more or less well studied cases include RNO 129 (Movsessian & Magakian 2004) and PV Cep (Movsessian et al 2008). The object V2494 Cyg, however, is the first FUor in this group, which makes it even more intriguing.…”

Section: The Starmentioning

confidence: 99%

V2494 Cyg: a unique FU Ori type object in the Cygnus OB7 complex

Magakian

Nikogossian

Movsessian

et al. 2013

Monthly Notices of the Royal Astronomical Society

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A photometric and spectral study of the variable star V2494 Cyg in the L 1003 dark cloud is presented. The brightness of the star, formerly known as HH 381 IRS, increased by 2.5 mag in R (probably in the 1980s) and since then has remained nearly constant. Since the brightness increase, V2494 Cyg has illuminated a bipolar cometary nebula. The stellar spectrum has several features typical of the FU Ori type, plus it exhibits very strong Hα and forbidden emission lines with high-velocity components. These emission lines originate in the HH jet near the star. The kinematic age of the jet is consistent with it forming at the time of the outburst leading to the luminosity increase. V2494 Cyg also produces a rather extended outflow; it is the first known FUor with both an observed outburst and a parsec-sized HH flow. The nebula, illuminated by V2494 Cyg, possesses similar morphological and spectral characteristics to Hubble's Variable Nebula (R Monocerotis/NGC 2261).

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“…Exposure times were between 90 and 180 s per image. The I C = 11.70 ± 0.04 mag on 2004 September 22 was derived from a CCD image obtained with the 2.6‐m telescope of Byurakan Observatory, Armenia, and shown in the paper of Movsessian et al (2008). The image of PV Cep was saturated, and its magnitude was derived by fitting the point spread function (PSF) to the unsaturated wing of the stellar image.…”

Section: Observationsmentioning

confidence: 99%

“…PV Cep was also observed with the IAC-80 telescope of the Teide Observatory (Spain) between 2009 October 25 and November 7. More detailed description of these instruments is given in Acosta-Pulido et al (2007) obtained with the 2.6-m telescope of Byurakan Observatory, Armenia, and shown in the paper of Movsessian et al (2008). The image of PV Cep was saturated, and its magnitude was derived by fitting the PSF to the unsaturated wing of the stellar image.…”

Section: Photometrymentioning

confidence: 99%

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Inner disc rearrangement revealed by dramatic brightness variations in the young star PV Cep

Kun

Szegedi-Elek

Moór

et al. 2011

Monthly Notices of the Royal Astronomical Society

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Young Sun‐like stars at the beginning of the pre‐main‐sequence (PMS) evolution are surrounded by accretion discs and remnant protostellar envelopes. Photometric and spectroscopic variations of these stars are driven by interactions of the star with the disc. Time‐scales and wavelength dependence of the variability carry information on the physical mechanisms behind these interactions. We conducted multi‐epoch, multiwavelength study of PV Cep, a strongly variable, accreting PMS star. By combining our own observations from 2004 to 2010 with archival and literature data, we show that PV Cep started a spectacular fading in 2005, reaching an IC‐band amplitude of 4 mag. Analysis of variation of the optical and infrared fluxes, colour indices and emission line fluxes suggests that the photometric decline in 2005–2009 resulted from an interplay between variable accretion and circumstellar extinction: since the central luminosity of the system is dominated by accretion, a modest drop in the accretion rate could induce the drastic restructuring of the inner disc. Dust condensation in the inner disc region might have resulted in the enhancement of the circumstellar extinction.

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Integral spectroscopy of the nebula GM 1-29 and the star PV Cep

Cited by 5 publications

References 12 publications

Hydrogen lines as a diagnostic tool for studying multicomponent emitting regions in hot young stars: magnetosphere, X-wind, and disk wind

Hydrogen lines as a diagnostic tool for studying multicomponent emitting regions in hot young stars: magnetosphere, X-wind, and disk wind

V2494 Cyg: a unique FU Ori type object in the Cygnus OB7 complex

Inner disc rearrangement revealed by dramatic brightness variations in the young star PV Cep

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