Echelle-mepsicron time-resolved spectroscopy of the dwarf nova SS Cygni

1987 ◽  
Vol 130 (1-2) ◽  
pp. 111-111
Author(s):  
J. Echevarria ◽  
F. Diego ◽  
M. Tapia ◽  
R. Costero
Keyword(s):  
Time Resolved ◽  
Time Resolved Spectroscopy ◽  
Dwarf Nova

scholarly journals Echelle-MEPSICRON time-resolved spectroscopy of the dwarf nova SS Cygni

1989 ◽  
Vol 240 (4) ◽  
pp. 975-990 ◽  
Author(s):  
J. Echevarria ◽  
F. Diego ◽  
M. Tapia ◽  
R. Costero ◽  
E. Ruiz ◽  
...  
Keyword(s):  
Time Resolved ◽  
Time Resolved Spectroscopy ◽  
Dwarf Nova

scholarly journals The Ultrashort Period Dwarf Nova SW Ursae Majoris

1987 ◽  
Vol 93 ◽  
pp. 125-126
Author(s):  
A.W. Shafter ◽  
J.A. Hill ◽  
E.L. Robinson ◽  
P. Szkody ◽  
J.R. Thorstensen ◽  
...  
Keyword(s):  
Wave Component ◽  
S Wave ◽  
Time Resolved ◽  
Time Resolved Spectroscopy ◽  
Dwarf Nova

AbstractSW UMa is an unusual dwarf nova in several respects. Recent observations by Robinson et al. (1986) have established that SW UMa is an SU UMa system, while Shafter, Szkody, and Thorstensen (1986) have presented evidence suggesting that SW UMa may be a DQ Her system as well. If the DQ Her classification is confirmed then SW UMa will be the only system to have this dual classification. Finally, time resolved spectroscopy of SW UMa has revealed the presence of an S-wave component in the Ha emission which has an unexpected phasing relative to the line wings.

scholarly journals Red Spectroscopy of IP Pegasi

1987 ◽  
Vol 93 ◽  
pp. 145-149
Author(s):  
J.S. Martin ◽  
D.H.P. Jones ◽  
R.C Smith
Keyword(s):  
Radial Velocity ◽  
Cross Correlation ◽  
Main Sequence ◽  
Mass Function ◽  
Velocity Curve ◽  
Absorption Lines ◽  
Radial Velocity Curve ◽  
Time Resolved ◽  
Time Resolved Spectroscopy ◽  
Dwarf Nova

AbstractTime resolved spectroscopy of the dwarf nova IP Pegasi in the range λλ 7670–8320Å shows absorption lines originating from the cool secondary. A radial velocity curve for this component has been derived by cross-correlation with a normal M star. The curve has semi-amplitude K2 = 288.3 ± 4 km s−1, and is slightly distorted. This distortion is equivalent to an orbit with an apparent eccentricity of 0.075 ± 0.024. The mass function of the primary is 0.394 ± 0.016M⊙. From this we derive constraints on the component masses of 0.62 < M1 < 1.14M⊙ and 0.17 < M2 < 0.71M⊙. The red star has a radius in the range 0.32 < R2 < 0.51R⊙ and is probably on the main sequence.

scholarly journals Photophysical properties and fluorosolvatochromism of D–π–A thiophene based derivatives

RSC Advances ◽  
2020 ◽  
Vol 10 (71) ◽  
pp. 43459-43471
Author(s):  
Hussain A. Z. Sabek ◽  
Ahmed M. M. Alazaly ◽  
Dina Salah ◽  
Hesham S. Abdel-Samad ◽  
Mohamed A. Ismail ◽  
...  
Keyword(s):  
Photophysical Properties ◽  
Fluorescence Emission ◽  
Time Resolved ◽  
Time Resolved Spectroscopy ◽  
Solvation Models

Solvation-dependent photophysical properties of two push–pull thiophene-based compounds with donor–π–acceptor (D–π–A) structures were investigated using absorption, fluorescence emission and time resolved spectroscopy, and supported by different solvation models.

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