High-velocity iron absorption lines in supernova remnant 1006

1983 ◽  
Vol 269 ◽  
pp. L5 ◽  
Author(s):  
C.-C. Wu ◽  
M. Leventhal ◽  
C. L. Sarazin ◽  
T. R. Gull
Keyword(s):  
High Velocity ◽  
Supernova Remnant ◽  
Iron Absorption ◽  
Absorption Lines

Ultraviolet Absorption Lines from High-Velocity Gas in the Vela Supernova Remnant: New Insights from Space Telescope Imaging Spectrograph Echelle Observations of HD 72089

1998 ◽  
Vol 492 (2) ◽  
pp. L147-L150 ◽  
Author(s):  
Edward B. Jenkins ◽  
Todd M. Tripp ◽  
Edward L. Fitzpatrick ◽  
Don Lindler ◽  
Anthony C. Danks ◽  
...  
Keyword(s):  
High Velocity ◽  
Supernova Remnant ◽  
Ultraviolet Absorption ◽  
Absorption Lines ◽  
Space Telescope ◽  
Imaging Spectrograph

scholarly journals High-velocity gas associated with the supernova remnant S147

1981 ◽  
Vol 195 (3) ◽  
pp. 485-495 ◽  
Author(s):  
A. P. Phillips ◽  
P. M. Gondhalekar ◽  
J. C. Blades
Keyword(s):  
High Velocity ◽  
Supernova Remnant

scholarly journals Interaction of high-velocity pulsars with supernova remnant shells

2003 ◽  
Vol 397 (3) ◽  
pp. 913-920 ◽  
Author(s):  
E. van der Swaluw ◽  
A. Achterberg ◽  
Y. A. Gallant ◽  
T. P. Downes ◽  
R. Keppens
Keyword(s):  
High Velocity ◽  
Supernova Remnant

scholarly journals High-velocity interstellar absorption associated with the supernova remnant W28

2020 ◽  
Vol 495 (3) ◽  
pp. 2909-2920 ◽  
Author(s):  
Adam M Ritchey
Keyword(s):  
High Velocity ◽  
Molecular Cloud ◽  
Supernova Remnant ◽  
Line Emission ◽  
Line Of Sight ◽  
Interstellar Gas ◽  
Lower Velocity ◽  
North East ◽  
The North ◽  
Visible Wavelengths

ABSTRACT We present an analysis of moderately high-resolution optical spectra obtained for the sightline to CD−23 13777, an O9 supergiant that probes high-velocity interstellar gas associated with the supernova remnant W28. Absorption components at both high positive and high negative velocity are seen in the interstellar Na i D and Ca ii H and K lines towards CD−23 13777. The high-velocity components exhibit low Na i/Ca ii ratios, suggesting efficient grain destruction by shock sputtering. High column densities of CH+, and high CH+/CH ratios, for the components seen at lower velocity may be indicative of enhanced turbulence in the clouds interacting with W28. The highest positive and negative velocities of the components seen in Na i and Ca ii absorption towards CD−23 13777 imply that the velocity of the blast wave associated with W28 is at least 150 km s−1, a value that is significantly higher than most previous estimates. The line of sight to CD−23 13777 passes very close to a well-known site of interaction between the supernova remnant and a molecular cloud to the north-east. The north-east molecular cloud exhibits broad molecular line emission, OH maser emission from numerous locations, and bright extended GeV and TeV γ-ray emission. The sightline to CD−23 13777 is thus a unique and valuable probe of the interaction between W28 and dense molecular gas in its environs. Future observations at ultraviolet and visible wavelengths will help to better constrain the abundances, kinematics, and physical conditions in the shocked and quiescent gas along this line of sight.

ChandraX‐Ray Observations of NGC 4258: Iron Absorption Lines from the Nucleus

2004 ◽  
Vol 601 (1) ◽  
pp. 133-141 ◽  
Author(s):  
A. J. Young ◽  
A. S. Wilson
Keyword(s):  
Iron Absorption ◽  
Absorption Lines

scholarly journals Hubble Space TelescopeObservations of High‐Velocity Lyα and Hα Emission from Supernova Remnant 1987A: The Structure and Development of the Reverse Shock

2003 ◽  
Vol 593 (2) ◽  
pp. 809-830 ◽  
Author(s):  
Eli Michael ◽  
Richard McCray ◽  
Roger Chevalier ◽  
Alexei V. Filippenko ◽  
Peter Lundqvist ◽  
...  
Keyword(s):  
High Velocity ◽  
Supernova Remnant ◽  
Reverse Shock ◽  
Hα Emission ◽  
Supernova Remnant 1987A

scholarly journals Stalled Winds: Interactions Between Nebulae and Stellar Winds

1989 ◽  
Vol 131 ◽  
pp. 456-456
Author(s):  
J. B. Kaler ◽  
W.A. Feibelman ◽  
R. A. Shaw ◽  
H. Henrichs
Keyword(s):  
High Velocity ◽  
Planetary Nebulae ◽  
Absorption Lines ◽  
Absorption Feature ◽  
Expansion Velocity ◽  
Stellar Winds ◽  
Low Velocity ◽  
Density Enhancement

Spectra of the nuclei of two planetaries show what appear to be features caused by fast stellar winds as they encounter the surrounding nebulae. Superimposed upon the high velocity (3670 km s−1) ultraviolet P Cygni profiles of Abell 78 are low velocity absorption lines that likely arise from a density enhancement in the wind as it brakes and builds up against the inner edge of the nebula. The deepest portions of these narrow absorptions fall at −78 km s−1 for N V and O V and −26 km s−1 for C IV, which implies a gradient in the decelerating wind, as does the profile of the strongest C IV line. The lower value may be related to the expansion velocity of the inner helium-rich nebulosity, which we associate with a sharp absorption feature. Another density enhancement, evidenced only by absorption lines, appears at −250 km s−1, and may be caused by a rebound shock of the sort envisioned by Kahn (IAU Symposium No. 103, Planetary Nebulae, 1983, 305) and Okorokov et al. (Astr. Ap., 1985, 142, 441).

scholarly journals FeII in the UV Spectrum of Luminous Emission Line Stars

1986 ◽  
Vol 116 ◽  
pp. 275-276
Author(s):  
G. Muratorio ◽  
M. Friedjung ◽  
R. Viotti
Keyword(s):  
Mass Loss ◽  
Emission Line ◽  
High Velocity ◽  
Previous Analysis ◽  
Magellanic Clouds ◽  
Absorption Lines ◽  
High Dispersion ◽  
Uv Spectrum ◽  
Loss Rates

Following the excessive mass loss rates we derived in a previous analysis of the FeII emission and absorption lines of some luminous Magellanic Clouds stars, assuming the two components formed in the same region (Muratorio et al., 1984), we again analysed the FeII data using the same method (Muratorio, 1985), but taking into account the presence of high velocity winds detected in some stars (R66, R126) by the study of the high dispersion IUE spectra (Stahl et al., 1983; Zickgraf et al., 1985).

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