Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 693734.0, MPI für Astronomie / Publikationen_mpia
Pre-main-sequence binaries with tidally disrupted discs: the Brγ in HD 104237
Authors:Garcia, P. J. V.; Benisty, M.; Dougados, C.; Bacciotti, F.; Clausse, J.-M.; Massi, F.; Mérand, A.; Petrov, R.; Weigelt, G.
Date of Publication (YYYY-MM-DD):2013
Title of Journal:Monthly Notices of the Royal Astronomical Society
Issue / Number:3
Start Page:1839
End Page:1853
Review Status:Internal review
Audience:Experts Only
Abstract / Description:Active pre-main-sequence binaries with separations of around 10 stellar radii present a wealth of phenomena unobserved in common systems. The study of these objects is extended from classical T Tauri stars to the Herbig Ae star HD 104237. The primary has a mass 2.2 ± 0.2 M and secondary 1.4 ± 0.3 M. Spectrointerferometry with the VLTI/AMBER in the K-band continuum and the Brγ line is presented. It is found that the K-band continuum squared visibilities are compatible with a circumbinary disc with a radius of ˜0.5 AU. However, a significant fraction (˜50 per cent) of the flux is unresolved and not fully accounted by the stellar photospheres. The stars probably do not hold circumstellar discs, in addition to the circumbinary disc, due to the combined effects of inner magnetospheric truncation and outer tidal truncation. This unresolved flux likely arises in compact structures inside the tidally disrupted circumbinary disc. Most (≳90 per cent) of the Brγ line emission is unresolved. The line-to-continuum spectroastrometry shifts in time, along the direction of the Lyα jet known to be driven by the system. The shift is anticorrelated with the Brγ equivalent width. It is shown that the unresolved Brγ emission cannot originate in the jet but instead is compatible with stellar emission from the orbiting binary components. The increase in the absolute value of the equivalent width of the line takes place at periastron passage; it could arise in an accretion burst, a flare or in the increase in effective size of the emission region by the interaction of the magnetospheres. The binary longitude of the ascending node is found to be Ω = (235 ± 3)° and the orbit retrograde. The origin of the jet is revisited. The tidal disruption of the circumstellar discs creates difficulties to ejection models that rely on stellar magnetosphere and disc coupling. A scenario of a stellar wind collimated by a circumbinary disc wind is suggested.
Free Keywords:accretion; accretion discs; binaries: spectroscopic; circumstellar matter; stars: individual: HD 104237; stars: pre-main-sequence; ISM: jets and outflows
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711 [ID No:1]
URL:http://cdsads.u-strasbg.fr/abs/2013MNRAS.430.1839G [ID No:2]
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.