Temporal Observations of the λ 5303 Emission Line Profile during the 74 Minute Totality from the Concorde SST at the 30 June 1973 Total Solar Eclipse: Preliminary Intensity Variations Above an Active Region

1974 ◽  
pp. 485-487
Author(s):  
D. H. Liebenberg ◽  
M. M. Hoffman
Keyword(s):  
Active Region ◽  
Emission Line ◽  
Line Profile ◽  
Solar Eclipse ◽  
Total Solar Eclipse ◽  
Emission Line Profile

FeXIV Line Emission Polarization of the July 11, 1991 Solar Corona

1994 ◽  
Vol 144 ◽  
pp. 541-547
Author(s):  
J. Sýkora ◽  
J. Rybák ◽  
P. Ambrož
Keyword(s):  
High Resolution ◽  
Solar Corona ◽  
Emission Line ◽  
Solar Eclipse ◽  
White Light ◽  
Preliminary Analysis ◽  
Line Emission ◽  
Total Solar Eclipse ◽  
Degree Of Polarization ◽  
High Resolution Images

AbstractHigh resolution images, obtained during July 11, 1991 total solar eclipse, allowed us to estimate the degree of solar corona polarization in the light of FeXIV 530.3 nm emission line and in the white light, as well. Very preliminary analysis reveals remarkable differences in the degree of polarization for both sets of data, particularly as for level of polarization and its distribution around the Sun’s limb.

Anomalous Hα Emission Line Profile Detected at the Center of DDO 53

2021 ◽  
Vol 919 (2) ◽  
pp. 73
Author(s):  
Justin A. Kader ◽  
Liese van Zee ◽  
Kristen B. W. McQuinn ◽  
Laura C. Hunter
Keyword(s):  
Emission Line ◽  
Line Profile ◽  
Hα Emission ◽  
Emission Line Profile

scholarly journals Emission-line-profile variability as a contraint on the structure and dynamics of hot star winds

2003 ◽  
Vol 212 ◽  
pp. 168-169
Author(s):  
Luc Dessart ◽  
Stanley P. Owocki
Keyword(s):  
Emission Line ◽  
Line Profile ◽  
Theoretical Calculations ◽  
Line Center ◽  
Radiation Hydrodynamics ◽  
Velocity Scale ◽  
Centre Region ◽  
Lateral Extent ◽  
Emission Line Profile ◽  
Hot Star Winds

We present theoretical calculations of emission-line-profile variability (LPV), based on radiation hydrodynamics simulations of the infamous radiative instability of hot star winds. We demonstrate that spherically symmetric wind structures (shells) cannot account for the observed profile variability at line center. Hence, we resort to a model that breaks-up the wind volume into a number of independent star-centered cones. The essential approximation made here is that each of these cones can be described by a structure calculated with a one-dimensional (1d) radiation hydrodynamics model. Such pseudo-3d ‘patch’-method leads to a satisfactory reproduction of the fundamental characteristics of LPV observed in O-type and Wolf-Rayet star optical spectra: the low-level fluctuations in the profile centre region, a migration of variable sub-peaks from line center to edge, that mimics the underlying wind acceleration. Our method highlights the correlation between the velocity scale of profile sub-peaks at line center and the lateral extent of wind structures, while at line edge it reflects the intrinsic radial velocity dispersion of emitting clumps. However, our model fails to reproduce the increase in this characteristic velocity scale from line center to edge, which we believe is a shortcoming of our purely 1d hydrodynamics approach.

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