SIMBAD references

2009A&A...505..695F - Astronomy and Astrophysics, volume 505, 695-706 (2009/10-2)

Results from DROXO. II. [NeII] and X-ray emission from ρ Ophiuchi young stellar objects.

FLACCOMIO E., STELZER B., SCIORTINO S., MICELA G., PILLITTERI I. and TESTI L.

Abstract (from CDS):

The infrared [NeII] and [NeIII] fine structure lines at 12.81 µm and 15.55 µm have recently been theoretically predicted to trace the circumstellar disk gas subject to X-ray heating and ionization. We observationally investigate the origin of the neon fine structure line emission by comparing observations with models of X-ray irradiated disks and by searching for empirical correlations between the line luminosities and stellar and circumstellar parameters. We select a sample of 28 young stellar objects in the ρ Ophiuchi star formation region for which good quality infrared spectra and X-ray data have been obtained, the former with the Spitzer/IRS and the latter with the deep rho Ophiuchi XMM-Newton observation (DROXO). We measure neon line fluxes and X-ray luminosities; we complement these data with stellar/circumstellar parameters obtained by fitting the spectral energy distributions of our objects (from optical to millimeter wavelengths) with star/disk/envelope models. We detect the [NeII] and the [NeIII] lines in 10 and 1 cases, respectively. Line luminosities show no correlation with X-ray emission. The luminosity of the [NeII] line for one star, and that of both the [NeII] and [NeIII] lines for a second star, match the predictions of published models of X-ray irradiated disks; for the remaining 8 objects the [NeII] emission is 1-3dex higher than predicted on the basis of their LX. However, the stellar/circumstellar characteristics assumed in published models do not match those of most of the stars in our sample. ClassI objects show significantly stronger [NeII] lines than ClassII and ClassIII ones. A correlation is moreover found between the [NeII] line emission and the disk mass accretion rates estimated from the spectral energy distributions. This might point toward a role of accretion-generated UV emission in the generation of the line or to other mechanisms related to mass inflows from circumstellar disks and envelopes and/or to the associated mass outflows (winds and jets). The X-ray luminosity is clearly not the only parameter that determines the [NeII] emission. For more exacting tests of X-ray irradiated disk models, these must be computed for the stellar and circumstellar characteristics of the observed objects. Explaining the strong [NeII] emission of ClassI objects likely requires the inclusion in the models of additional physical components such as the envelope, inflows, and outflows.

Abstract Copyright:

Journal keyword(s): stars: activity - stars: formation - stars: circumstellar matter - stars: planetary systems: protoplanetary disks - stars: pre-main sequence

CDS comments: CRBR 85 is CRBR 2422.8-3423 in Simbad.

Simbad objects: 62

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2019.10.18-04:56:56

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