UV spectral variability in the Herbig Ae star HR 5999
Read Online
Share

UV spectral variability in the Herbig Ae star HR 5999

  • 600 Want to read
  • ·
  • 44 Currently reading

Published by National Aeronautics and Space Administation in [Washington, D.C.? .
Written in English

Subjects:

  • Accretion (Astrophysics),
  • Ultraviolet astronomy.

Book details:

Edition Notes

Other titlesAccretion interpretation.
StatementM.R. Pe rez, C.A. Grady, and P.S. The .
Series[NASA contractor report] -- NASA CR-189313.
ContributionsGrady, C. A., The , P. S., United States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL14705596M

Download UV spectral variability in the Herbig Ae star HR 5999

PDF EPUB FB2 MOBI RTF

The variable Herbig AE star HR IX - Variability in the UV shell lines Article (PDF Available) in Astronomy and Astrophysics Supplement Series September with 11 Reads. A&A manuscript no. (will be inserted by hand later) Your thesaurus codes are: 07() ASTRONOMY AND ASTROPHYSICS! NASA CR UV spectral variability in the Herbig Ae star HR HR has a spectral type of A7 III-IV and forms a ∼ 45′′ wide proper-motion binary system with the A star HR The Hipparcos parallax for HR corresponds to a distance of +50 −30 pc. The spectral energy distribution of HR shows a clear infrared excess at wavelengths above 1µm. IRAS detected HR at 12, 25, and 60µm, but pro-. Analysis of IUE high- and low-dispersion spectra of the young Herbig Ae star HR (HD ) covering – has revealed dramatic changes in the Mg II h and k (, Å) emission profiles, changes in the column density and distribution in radial velocity of accreting gas, and flux in the Lyα, OI and CIV emission lines, which are correlated with the UV excess : M. R. Pérez, C. A. Grady.

Spectral Type: A 7 IV e L bol = L o, A V = mag M = M o, age = Myr HR v sin i = km/sec HR 12’ x 12’ K + R + B Properties of HR (alias HD , V Sco): HR SpT = A no emission lines no infrared excess Ænot a Herbig star! Infrared excess: circumstellar mass ~ M o. Analysis of IUE high- and low-dispersion spectra of the young Herbig Ae star HR (HD ) covering has revealed dramatic changes in the Mg II h and k (, Å) emission profiles, changes in the column density and distribution in radial velocity of accreting gas, and flux in the Lyα, OI and CIV emission lines, which are correlated with the UV excess luminosity. IUE observations are noted to indicate that HD exhibits the same UV, visible, and IR spectral properties as the Herbig Ae stars AB Aur and HR It is accordingly concluded that HD. environment surrounding Herbig Ae stars. Aims. We present new long-baseline spectro-interferometric observations of the Herbig Ae star, HR , obtained in the H and K bands with the AMBER instrument at the VLTI, and aim to produce near-infrared images at the sub-AU spatial scale. by:

UV spectral variability in the Herbig Ae star HR XI, The accretion interpretation. [M R Pérez; C A Grady; P S Thé; United States. National Aeronautics and Space Administration.]. Abstract. Analysis of IUE high- and low-dispersion spectra of the young Herbig Ae star HR (HD ) covering revealed dramatic changes in the Mg II h and k (, A) emission profiles, changes in the column density and distribution in radial velocity of accreting gas, and flux in the Ly(alpha), O I, and C IV emission lines, which are correlated with the UV excess Author: M. R. Perez, C. A. Grady and P. S. The. Herbig Ae/Be stars are intermediate-mass pre-main sequence stars surrounded by circumstellar dust disks. Some are observed to produce jets, whose appearance as a sequence of shock fronts (knots) suggests a past episodic outflow by: A Statistical SpectropolarimetricStudy of Herbig Ae/Be Stars troscopic variability that a Herbig Ae star is currently undergo- Fairlamb et al. () found that the UV-excess of Herbig Ae stars can be explained by magnetospheric accretion, but that the earliest Herbig Be stars have too large UV .