High-resolution ultraviolet spectrograph for sounding rocket measurements of planetary emission line profiles

1993 ◽  
Vol 32 (12) ◽  
pp. 3016 ◽  
Author(s):  
Walter M. Harris
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Sounding Rocket ◽  
Line Profiles ◽  
Rocket Measurements

A high resolution UV spectrograph for sounding rocket measurement of planetary emission line profiles

1992 ◽  
Author(s):  
Walter M. Harris ◽  
John T. Clarke ◽  
Jack Caldwell ◽  
Paul D. Feldman ◽  
Brett C. Bush ◽  
...  
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Sounding Rocket ◽  
Line Profiles ◽  
Rocket Measurement

High Resolution Emission Line Profiles in Blue Luminous Stars

1989 ◽  
pp. 279-280 ◽  
Author(s):  
Rino Bandiera ◽  
Paola Focardi ◽  
Aldo Altamore ◽  
Corrine Rossi ◽  
Otmar Stahl
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Line Profiles

scholarly journals High-resolution emission line profiles in blue luminous stars

1989 ◽  
Vol 113 ◽  
pp. 279-280
Author(s):  
Rino Bandiera ◽  
Paola Focardi ◽  
Aldo Altamore ◽  
Corinne Rossi ◽  
Otmar Stahl
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
High Velocity ◽  
Large Scale ◽  
Velocity Fields ◽  
Emission Lines ◽  
Line Profiles ◽  
High Luminosity ◽  
Stellar Envelopes ◽  
Η Car

Emission lines are often observed in high luminosity stars and provide evidence of the presence of extended stellar envelopes. Ha is the most frequently observed across the H-R diagram, but lines of Hel or Fell are also found in emission in these stars. They could be used as diagnostics of the structure of their outer atmospheres and winds. High resolution (1/dl ~ 105) high S/N profiles of Ha and Hel 5876 in the galactic LBVs η Car, AG and HR Car, and in the LMC star S22 have been obtained with the ESO CAT-CES during 1984-87, and are described in Figs.1-5. We find that these stars show a large variety of profiles with narrow and broad emissions, wide or multiple blue-shifted absorptions. The profiles are largely variable. Once, a kind of inverse P Cyg profile was observed in HR Car (Fig.4). These results indicate the presence of large scale phenomena and high velocity fields which are dramatically variable in time. Continuous HIRES monitoring of these stars is urgently needed.

scholarly journals High-Resolution Emission-Line Spectroscopy of Be Stars: Comparison of Hα and Weak Emission Lines

1987 ◽  
Vol 92 ◽  
pp. 208-210
Author(s):  
Reinhard W. Hanuschik
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Rotational Velocity ◽  
Outer Radius ◽  
Emission Lines ◽  
Be Stars ◽  
Line Profiles ◽  
Component Structure ◽  
Double Peak Structure ◽  
Disk Component

AbstractFor a number of bright southern Be stars, high-resolution, high S/N spectroscopy has been performed for Hα, Si II λ6371 and four Fe II emission lines. With the exception of four stars, both Hα and weak emission line profiles exhibit resolved double-peak structure. Peak separation increases with stellar projected rotational velocity. In many cases, Hα profiles (but not Fe II lines) show resolved fine-structure (inflections in the flanks) indicating a two-component structure of the disk. Envelope models with arbitrary density and rotational velocity laws have been fitted to the Fe II line profiles with satisfactory results. It is found that the innermost Hα disk component also emits the Fe II lines and has an average outer radius of 5 r*; density falls off as r-l.5 or more rapidly. The outer disk component emits the faint and narrow secondary component of Hα lines with average outer radius 20 r*. The envelopes of the four stars with a strong, dominating single peak both in Hα and Fe II either are dominated by strong radial motions or, more likely, have elliptical disk-like structure.

scholarly journals Substructures in the Narrow-Line Region of AGN

1989 ◽  
Vol 134 ◽  
pp. 312-313
Author(s):  
Sylvain Veilleux
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Seyfert Galaxies ◽  
Narrow Line ◽  
Line Profiles ◽  
Preliminary Results ◽  
Line Region ◽  
Narrow Line Region ◽  
Narrow Emission ◽  
Resolution Study

The preliminary results of a high-resolution study of narrow emission-line profiles in bright Seyfert galaxies are reported. Profile substructures such as secondary peaks and shoulders are observed in nearly all the objects. The results of profile comparisons in Mrk 359, Mrk 533, and Mrk 1066 are briefly discussed.

scholarly journals Theoretical Narrow Emission-Line Profiles of Active Galactic Nuclei

1989 ◽  
Vol 134 ◽  
pp. 318-319
Author(s):  
M. Contini ◽  
S.M. Viegas-Aldrovandi
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Active Galactic Nuclei ◽  
Line Profile ◽  
Galactic Nuclei ◽  
Line Profiles ◽  
Narrow Emission

In recent years, a large number of high resolution observations of active galactic nuclei (AGN) have become available. Most of them show the [OIII]5007 line profile (Heckman, Miley and Green 1984, Vrtilek and Carleton 1985, Whittle 1985a,b).

scholarly journals Emission Line Profiles in the Planetary Nebulae IC 4593 and NGC 6153

1989 ◽  
Vol 131 ◽  
pp. 189-189
Author(s):  
D.P.K. Banerjee ◽  
B. G. Anandarao
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Planetary Nebulae ◽  
Central Star ◽  
Compact Objects ◽  
Emission Lines ◽  
Complex Structures ◽  
Line Profiles ◽  
Fabry Perot ◽  
Central Regions

The Planetary Nebulae IC 4593 and NGC 6153 are two rather compact objects not well studied. The nebula IC 4593 is about 12 arcsec in diameter and has a central star of Type 07 f; while the southern nebula NGC 6153 is about 22 arcsec in diameter and its central star is faint and of unknown spectral type. Using a high-resolution scanning Fabry-Pérot spectrometer we have made profile measurements of emission lines Hα λ6563 A, [O III] λ5007 A, and [N II] λ6584 A in the central regions of these two nebulae. We have found expansion velocities for IC 4593 of 40 km s−1 in [N II] and 16 km s−1 in [O III]. In the case of NGC 6153, we have obtained expansion velocities of 15 km s−1 in [N II] and 13 km s−1 in [O III] line. The profiles in Hα in both the nebulae dis not show a double peaked feature due to the larger thermal broadening. In the case of IC 4593, both [O III] and [N II] profiles showed complex structures. These results and their interpretation will be discussed.

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.

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