Parameters of broadening of water molecule absorption lines by argon derived using different line profile models

2017 ◽  
Vol 30 (2) ◽  
pp. 123-128 ◽  
Author(s):  
T. M. Petrova ◽  
A. M. Solodov ◽  
A. P. Shcherbakov ◽  
V. M. Deichuli ◽  
A. A. Solodov ◽  
...  
Keyword(s):  
Water Molecule ◽  
Line Profile ◽  
Absorption Lines

Non-L.T.E. and Scattering Effects on the Strong-Line Profiles of Sodium

1967 ◽  
Vol 1 (1) ◽  
pp. 9-10
Author(s):  
D. Mugglestone
Keyword(s):  
Line Profile ◽  
Solar Atmosphere ◽  
Absorption Lines ◽  
Strong Line ◽  
Line Profiles ◽  
Solar Absorption ◽  
Physical Conditions ◽  
Scattering Effects ◽  
The University ◽  
Work Done

I am reporting here work done recently by the astrophysics group at the University of Queensland (notably G. D. Finn and R. L. Young). We are interested in the detailed formation of the profiles of the sodium-D solar absorption lines. These lines are very strong with extended wings and the object of the exercise is to determine how closely, under the physical conditions assumed to exist in the solar atmosphere, we can theoretically reproduce the detailed line profile which is observed.

scholarly journals Non-radial Pulsation Modeling of ω (28) CMa

2000 ◽  
Vol 175 ◽  
pp. 244-247 ◽  
Author(s):  
M. Maintz ◽  
Th. Rivinius ◽  
S. Tubbesing ◽  
B. Wolf ◽  
S. Štefl ◽  
...  
Keyword(s):  
Velocity Field ◽  
Line Profile ◽  
Inertial Frame ◽  
Absorption Lines ◽  
Pulsation Period ◽  
Radial Pulsation ◽  
Line Profiles ◽  
Stellar Rotation ◽  
Velocity Effect

AbstractAdopting non-radial pulsation (nrp) the line profile variability lpv of several absorption lines of different ions was modeled for ω (28) CMa. The parameters suggested by Baade (1982) to characterise the pulsation could be confirmed. The pulsation period in the inertial frame was found to be negative, i.e. an actually retrograde mode appears prograde due to the rapid stellar rotation. The line profiles could be reproduced in detail including structures like spikes and ramps. They were identified as velocity effect due to the latitudinal component of the nrp velocity field υϑ in combination with low inclination i. In spite of small photometric variations (Štefl et al. 1999) the lpv of the absorption lines can be explained by nrp entirely.

Dicke Narrowing, Pressure Dependence, and Mixing of Self-Broadened CO2 Absorption Lines in the 30013 ← 00001 Band: Measurements and Line Profile Testing

2021 ◽  
Vol 34 (5) ◽  
pp. 381-389
Author(s):  
V. A. Kapitanov ◽  
K. Yu. Osipov ◽  
A. E. Protasevich ◽  
Yu. N. Ponomarev ◽  
Ya. Ya. Ponurovskii
Keyword(s):  
Line Profile ◽  
Pressure Dependence ◽  
Absorption Lines ◽  
Co2 Absorption

scholarly journals Is λ Cep a pulsating star?

2014 ◽  
Vol 9 (S307) ◽  
pp. 237-238
Author(s):  
J.M. Uuh-Sonda ◽  
P. Eenens ◽  
G. Rauw
Keyword(s):  
Absorption Line ◽  
Line Profile ◽  
Stellar Surface ◽  
Absorption Lines ◽  
Full Dataset ◽  
Rotating Star ◽  
Radial Pulsations

AbstractIt has been proposed that the variability seen in absorption lines of the O6Ief star λ Cep is periodical and due to non-radial pulsations (NRP). We have obtained new spectra during six campaigns lasting between five and nine nights. In some datasets we find recurrent spectral variations which move redward in the absorption line profile, consistent with perturbations on the stellar surface of a rotating star. However the periods found are not stable between datasets, at odds with the NRP hypothesis. Moreover, even when no redward trend is found in a full dataset of an observing campaign, it can be present in a subset, suggesting that the phenomenon is short-lived, of the order of a few days, and possibly linked to transient magnetic loops.

Two Modes of Pulsation in the Rapidly Rotating O9.5 Dwarf, HD 93521

1995 ◽  
Vol 155 ◽  
pp. 309-310
Author(s):  
A.H.N. Reid ◽  
D. Bohlender ◽  
C.T. Bolton ◽  
A.W. Fullerton ◽  
I.D. Howarth ◽  
...  
Keyword(s):  
Time Series ◽  
Time Series Analysis ◽  
Line Profile ◽  
Absorption Lines ◽  
Radial Pulsation ◽  
Preliminary Results ◽  
Series Analysis ◽  
The Continuum

AbstractWe present preliminary results of a time-series analysis on the He II λ4541Å, Si III λλ4552, 4567, 4575Å and Hβ λ486lÅ lines of the late O-type dwarf, HD 93521. The spectra show line-profile variations (lpv) − ‘bumps’ and ‘dips’ − of amplitude ∼ 1% of the continuum, moving systematically redwards through the photospheric absorption lines. The analysis implies non-radial pulsation (NRP) as the origin for the lpv.

Contrast of Filament Bright Rims

1994 ◽  
Vol 144 ◽  
pp. 365-367
Author(s):  
E. V. Kononovich ◽  
O. B. Smirnova ◽  
P. Heinzel ◽  
P. Kotrč
Keyword(s):  
High Altitude ◽  
Line Profile ◽  
Line Center ◽  
Magnetic Structures ◽  
The Mean

AbstractThe Hα filtergrams obtained at Tjan-Shan High Altitude Observatory near Alma-Ata (Moscow University Station) were measured in order to specify the bright rims contrast at different points along the line profile (0.0; ± 0.25; ± 0.5; ± 0.75 and ± 1.0 Å). The mean contrast value in the line center is about 25 percent. The bright rims interpretation as the bases of magnetic structures supporting the filaments is suggested.

Frequency Redistribution Effects in the Formation of Lyman α in Prominences and Their Influence on the Ratio of Hα to Lα

1979 ◽  
Vol 44 ◽  
pp. 53-55
Author(s):  
R.W. Milkey ◽  
J.N. Heasley ◽  
E.J. Schmahl ◽  
O. Engvold
Keyword(s):  
Line Profile ◽  
Large Fraction ◽  
Partial Frequency ◽  
Frequency Redistribution ◽  
Partial Frequency Redistribution ◽  
Emergent Intensity

The effect of partial frequency redistribution in the formation of Lyman α in the chromosphere has been discussed by Milkey and Mihalas (1973) and others, and it has been shown that in this case the coherency of scattering in the wings of the line substantially influences the line profile. Although there are non-negligible sources for La photons within a prominence, a large fraction of the emergent line photons are due to scattering of photons incident on the surface of the prominence so that one expects that in a prominence the frequency redistribution processes will play an important role in determining the emergent intensity.

Microstructure of post-deformed ECAP-Ti investigated by Multiple X-Ray Line Profile Analysis

2006 ◽  
Vol 2006 (suppl_23_2006) ◽  
pp. 129-134 ◽  
Author(s):  
E. Schafler ◽  
K. Nyilas ◽  
S. Bernstorff ◽  
L. Zeipper ◽  
M. Zehetbauer ◽  
...  
Keyword(s):  
Line Profile ◽  
Profile Analysis ◽  
Line Profile Analysis ◽  
X Ray
Sign in / Sign up

Export Citation Format

Share Document