[ITAL]Chandra[/ITAL] Detection of a Close X-Ray Companion and Rich Emission-Line Spectrum in the Wolf-Rayet Binary γ Velorum

2001 ◽  
Vol 558 (2) ◽  
pp. L113-L116 ◽  
Author(s):  
Stephen L. Skinner ◽  
Manuel Güdel ◽  
Werner Schmutz ◽  
Ian R. Stevens
Keyword(s):  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

scholarly journals The May 1985 Superoutburst of OY Carinae: II. Phase-Resolved IUE Spectroscopy and Exosat Observations

1987 ◽  
Vol 93 ◽  
pp. 371-376 ◽  
Author(s):  
B.J.M. Hassall ◽  
T. Naylor ◽  
G.T. Bath ◽  
P.A. Charles ◽  
G. Sonneborn ◽  
...  
Keyword(s):  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Dwarf Nova ◽  
Uv Emission ◽  
Emission Line Spectrum ◽  
Coronal Region

AbstractWe present ultraviolet and X-ray observations of the eclipsing SU UMa dwarf nova OY Car early in the decline from a superoutburst. From the UV emission line spectrum and lack of X-ray eclipse, we deduce the presence of an extended coronal region.

scholarly journals An X-ray emission-line spectrum of Nova V382 Velorum 1999

2005 ◽  
Vol 364 (3) ◽  
pp. 1015-1024 ◽  
Author(s):  
J.- U. Ness ◽  
S. Starrfield ◽  
C. Jordan ◽  
J. Krautter ◽  
J. H. M. M. Schmitt
Keyword(s):  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

scholarly journals X‐Ray–Irradiated Protoplanetary Disk Atmospheres. I. Predicted Emission‐Line Spectrum and Photoevaporation

2008 ◽  
Vol 688 (1) ◽  
pp. 398-407 ◽  
Author(s):  
Barbara Ercolano ◽  
Jeremy J. Drake ◽  
John C. Raymond ◽  
Cathie C. Clarke
Keyword(s):  
Emission Line ◽  
Protoplanetary Disk ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

Observation of the Solar Flare X-Ray Emission-Line Spectrum of Iron from 1.3 to 20 Å

1967 ◽  
Vol 149 ◽  
pp. L79 ◽  
Author(s):  
W. M. Neupert ◽  
W. Gates ◽  
M. Swartz ◽  
R. Young
Keyword(s):  
Solar Flare ◽  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

X-Ray Emission Line Spectrum of a Coronal Active Region

Nature ◽  
1967 ◽  
Vol 214 (5083) ◽  
pp. 41-42 ◽  
Author(s):  
K. EVANS ◽  
K. A. POUNDS ◽  
J. L. CULHANE
Keyword(s):  
Active Region ◽  
Emission Line ◽  
Line Spectrum ◽  
X Ray ◽  
Emission Line Spectrum

scholarly journals The Ionization of Novae Ejecta

1990 ◽  
Vol 122 ◽  
pp. 215-227
Author(s):  
R.E. Williams
Keyword(s):  
Emission Line ◽  
White Dwarf ◽  
Line Spectrum ◽  
Ionized Gas ◽  
Grain Formation ◽  
Emission Line Spectrum ◽  
Pass Through

AbstractNovae ejecta pass through four distinct phases of evolution of the emission-line spectrum, caused by different ionization characteristics of the shell. These include a neutral (I), an auroral (II), a coronal (III), and a nebular (IV) phase. Photoionization from the contracting photosphere of the hot white dwarf is the source of the ionization, including the highly ionized coronal phase. Changing emission line ratios in certain novae that develop dust are caused by condensation of grains from the gas, and can be used to determine the composition of the dust. In V1370 Aql, substantial silicate grain formation appears to have taken place, probably within the ionized gas.

scholarly journals The unusual emission line spectrum of I Zw 1

2004 ◽  
Vol 2004 (IAUS222) ◽  
pp. 271-274
Author(s):  
Monique Joly ◽  
M.-P. Véron-Cetty ◽  
P. Véron
Keyword(s):  
Emission Line ◽  
Line Spectrum ◽  
Emission Line Spectrum

scholarly journals Models for the Emission-Line Spectra of the Low-Excitation Herbig-Haro Objects

1987 ◽  
Vol 115 ◽  
pp. 346-347
Author(s):  
Michael A. Dopita ◽  
Saul Caganoff ◽  
Richard D. Schwartz ◽  
Martin Cohen
Keyword(s):  
Emission Line ◽  
Theoretical Description ◽  
Line Spectrum ◽  
High Excitation ◽  
Two Photon ◽  
Shock Models ◽  
Uv Excess ◽  
Hh Objects ◽  
Emission Line Spectrum

The class of Low-Excitation Herbig-Haro Objects are characterised by [SII] and [OI] lines which are comparable in strength to H-Alpha, by [NI] lines that are comparable to H-Beta, relatively weak [NII] and [OII] lines, little or no [OIII] emission and a very strong blue-UV “excess”. This blue and UV continuum in low-excitation HH Objects was noted as a problem by Brugel, Böhm and Mannery (1981), Ortalani and D'Odorico (1980) and Böhm, Böhm-Vitense and Brugel (1981). The first suggestion that it results from collisionally enhanced Hydrogen two-photon (2q) continuum was by Dopita (1981). The subsequent observations of Dopita, Binette and Schwartz (1982) proved that this was indeed the case. However, although very close correlations between this enhancement and the emission-line spectrum were found, a fair theoretical description could only be obtained for very youthful shock models with ages of order 30 years. However, there seems to be no reason why low excitation HH shocks should be much younger than the high excitation shocks.

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