Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/25985
Share/Export:
logo share SHARE logo core CORE BASE
Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL | DATACITE
Title

Hubble space telescope stis spectrum of RW Aurigae A.: evidence for an ionized beltlike structure and mass ejection in timescales of a few hours

AuthorsGómez de Castro, Ana Inés CSIC ORCID; Verdugo, Eva
KeywordsRW Aurigae
Stars
Ultraviolet observations
Astrophysics
Issue Date2003
PublisherAmerican Astronomical Society
CitationAstrophysical Journal, 597, 443-454 (2003)
AbstractProfiles of the UV semiforbidden lines of C iii]1908 and Si iii]1892 of RW Aur have been obtained with the Hubble Space Telescope (HST) STIS. The C iii]1908 profile shows two high-velocity components at v = ± 170 km s-1 and a central one. The Si iii]1892 profile is very broad (FWHM = 293 km s_1), and the high-velocity components are unresolved. The high-velocity components are most probably produced in a rotating belt similar to that detected in other sources of bipolar outflows. A radius between 2.7 R* and the corotation radius (6.1 R*) is derived, and a log Te (K)≈4:7 and log ne (cm-3) = 11:6 are estimated. The belt is clumpy, and the most likely source of heating is local X-ray radiation, probably associated with the release of magnetic energy. In addition, profiles of the optical lines of He i, Fe ii, and H_ retrieved from the HST archive have been analyzed. The spectra were obtained by shifting the STIS slit between exposures in the transverse direction to the flow. Two features vary from one exposure to another: a blueshifted emission feature (detected in the Fe ii and He i lines) and a redshifted absorption feature (detected in H_), which are observed at the velocity of the blueshifted and redshifted components of the jet, respectively. There is a clear-cut correlation between the equivalent widths of these two components. These components are not associated with the flaring activity of the source, since they remain stable timescales of ’40 minutes. They are most likely associated with variations in the stellar/circumstellar environment in timescales of a few (’5) hours, consistent with reports by other authors for variations of the veiling and the appearance of shell signature in the optical spectrum.
Publisher version (URL)http://dx.doi.org/10.1086/378381
URIhttp://hdl.handle.net/10261/25985
DOI10.1086/378381
ISSN0004-637X
E-ISSN1538-4357
Appears in Collections:(IAG) Artículos




Files in This Item:
File Description SizeFormat
articulo26_2003.pdf339,81 kBAdobe PDFThumbnail
View/Open
Show full item record
Review this work

SCOPUSTM   
Citations

30
checked on May 24, 2022

WEB OF SCIENCETM
Citations

27
checked on May 27, 2022

Page view(s)

405
checked on May 27, 2022

Download(s)

249
checked on May 27, 2022

Google ScholarTM

Check

Altmetric

Dimensions


WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.