scholarly journals Stellar wind flows in T Tauri stars

1987 ◽  
Vol 122 ◽  
pp. 105-106
Author(s):  
C. Sá ◽  
M.T.V.T. Lago ◽  
M.V. Penston
Keyword(s):  
Stellar Wind ◽  
General Pattern ◽  
T Tauri Stars ◽  
Emission Lines ◽  
High Dispersion ◽  
T Tauri ◽  
Wind Flows ◽  
Using Data

Following the successful modelling of the wind from RU Lupi using data at moderate and high dispersion we report on similar observations of other T Tauri stars where the general pattern of the wind, as deduced from the widths of the emission lines of the various species, seems to be similar.

scholarly journals Emission-line widths and stellar-wind flows in T Tauri stars

1986 ◽  
Vol 222 (2) ◽  
pp. 213-221 ◽  
Author(s):  
C. Sá ◽  
M. V. Penston ◽  
M. T. V. T. Lago
Keyword(s):  
Emission Line ◽  
Stellar Wind ◽  
T Tauri Stars ◽  
T Tauri ◽  
Wind Flows ◽  
Line Widths

Stellar Wind Flows in T Tauri Stars

1987 ◽  
pp. 105-106
Author(s):  
C. Sá ◽  
M. T. V. T. Lago ◽  
M. V. Penston
Keyword(s):  
Stellar Wind ◽  
T Tauri Stars ◽  
T Tauri ◽  
Wind Flows

scholarly journals Oh Observations Near the Reflection Nebulae Ngc 2068 and Ngc 2071

1974 ◽  
Vol 60 ◽  
pp. 301-302
Author(s):  
L. E. B. Johansson ◽  
B. Höglund ◽  
A. Winnberg ◽  
Nguyen-Q-Rieu ◽  
W. M. Goss
Keyword(s):  
Dust Cloud ◽  
T Tauri Stars ◽  
Emission Lines ◽  
Class I ◽  
Reflection Nebula ◽  
Cosmic Background ◽  
T Tauri ◽  
Reflection Nebulae

Narrow OH emission lines at 1667 MHz, apparently from a Class I source, have been observed near the reflection nebula NGC 2071. The region contains many T Tauri stars. OH emission corresponding to the dust cloud north and east of NGC 2024 is also seen. At 1720 MHz the dust cloud component appears in absorption; presumably the isotropic 2.7 K cosmic background is being absorbed.

scholarly journals Quasicyclic Light Changes in Three Low Mass T Tauri Stars

1977 ◽  
Vol 42 ◽  
pp. 66-71
Author(s):  
H. Mauder
Keyword(s):  
Variable Stars ◽  
T Tauri Stars ◽  
Emission Lines ◽  
T Tauri ◽  
Cyclic Variations ◽  
Low Mass ◽  
Photographic Survey ◽  
Objective Prism

During a photographic survey of the Chamaeleon T association in 1971/1972, evidence was found for quasiperiodic light changes of three variable stars, see Mauder and Sosna (1975). The period of 6.2 days for SY Cha is well seen, the periods of 7 days for VZ Cha and of 8 days for TW Cha are less pronounced. Intrinsic variations are present in addition to the cyclic variations. The three stars were classified by Hoffmeister (1963) as T Tauri type stars from their light variations. Objective prism spectra obtained by Henize and Mendoza (1973) confirm this classification, they found conspicuous emission lines. For SY Cha and TW Cha they got slit spectra, too, which show the typical veiling. The stars SY Cha, TW Cha and VZ Cha have been observed in the UBV system from 1974 March 12 until 1974 March 22, using the ESO standard photometer. In Figures 1 - 3 the light and colour curves are given for SY Cha, TH Cha and VZ Cha. Each point is a mean of generally 8 to 12 integrations, each integration lasting 5 seconds.

scholarly journals High Quality Echelle Observations of T Tauri Stars

1988 ◽  
Vol 132 ◽  
pp. 99-104
Author(s):  
G. Basri
Keyword(s):  
High Resolution ◽  
Line Profile ◽  
T Tauri Stars ◽  
Young Stars ◽  
Emission Lines ◽  
Current Understanding ◽  
General Nature ◽  
High Quality ◽  
T Tauri ◽  
Made In

This is a very brief review of the high resolution line profile work that has been done on very young stars. The spectral anamolies peculiar to these stars are mentioned, with some discussion of what may give rise to them. The Hα line is discussed most extensively, as the most work has been done with it. While progress has been made in understanding the general nature of T Tauri spectra, there are very large gaps in our current understanding of the emission lines from these stars.

Two New T Tauri stars and a Candidate FU Orionis Star associated with Bok Globules

1997 ◽  
Vol 163 ◽  
pp. 839-839
Author(s):  
J. L. Yun ◽  
M. Moreira
Keyword(s):  
Infrared Emission ◽  
T Tauri Stars ◽  
Emission Lines ◽  
Young Stellar Objects ◽  
Spectral Energy ◽  
Energy Distributions ◽  
Stellar Objects ◽  
T Tauri ◽  
Bok Globules ◽  
Reflection Nebulae

AbstractWe present photometric and spectroscopic evidence of two new T Tauri stars formed in the conditions of isolated small Bok globules. The spectral energy distributions of these objects display excess infrared emission, they are associated with optical reflection nebulae, and their optical spectra reveal Balmer emission lines and the Li I λ6707 Å absorption line. Additionnally, we report the discovery of what is likely to be a new FU Orionis star seen towards Bok globule CB34. The star is about 4 magnitudes brighter than it appears on the Palomar plates and is associated with the aggregate of young stellar objects forming in Bok globule CB34.

Magnetospheric Accretion Models for the Hydrogen Emission Lines of T Tauri Stars

1998 ◽  
Vol 492 (2) ◽  
pp. 743-753 ◽  
Author(s):  
James Muzerolle ◽  
Nuria Calvet ◽  
Lee Hartmann
Keyword(s):  
T Tauri Stars ◽  
Emission Lines ◽  
Hydrogen Emission ◽  
T Tauri ◽  
Hydrogen Emission Lines ◽  
Magnetospheric Accretion
Sign in / Sign up

Export Citation Format

Share Document