7.1.6 Radio line emission and absorption

Flares of Radio Line Emission H2O in ORI A and W49N

Flare Stars in Star Clusters, Associations and the Solar Vicinity ◽

10.1007/978-94-009-0607-5_56 ◽

1990 ◽

pp. 275-278

Author(s):

I. V. Gosachinskij ◽

N. A. Yudaeva ◽

R. A. Kandalian ◽

F. S. Nazaretian ◽

V. A. Sanamian

Keyword(s):

Line Emission ◽

Radio Line

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“Thermal” SiO radio line emission towards M-type AGB stars: A probe of circumstellar dust formation and dynamics

Astronomy and Astrophysics ◽

10.1051/0004-6361:20031068 ◽

2003 ◽

Vol 411 (2) ◽

pp. 123-147 ◽

Cited By ~ 98

Author(s):

D. González Delgado ◽

H. Olofsson ◽

F. Kerschbaum ◽

F. L. Schöier ◽

M. Lindqvist ◽

...

Keyword(s):

Line Emission ◽

Circumstellar Dust ◽

Dust Formation ◽

Agb Stars ◽

Radio Line

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Flares of radio line emission H2O in Ori A and W49N

Symposium - International Astronomical Union ◽

10.1017/s0074180900187856 ◽

1990 ◽

Vol 137 ◽

pp. 275-278

Author(s):

I.V. Gosachinskij ◽

N.A. Yudaeva ◽

R.A. Kandalian ◽

F.S. Nazaretian ◽

V.A. Sanamian

Keyword(s):

Radio Telescope ◽

Line Emission ◽

Light Curves ◽

Time Behaviour ◽

Velocity Range ◽

Radio Line ◽

Total Luminosity ◽

First Time ◽

Maser Sources ◽

Water Maser

The results of observations of H2O maser sources Ori A and W49N at 1.35cm made the RATAN-600 radio telescope from June 1981 till December 1988 are presented. The light curves of these sources showed several outbursts. Duration of the strongest outbursts for the Ori A and W49N are approximately 1 and 1.5yr respectively. The maximum of the total luminosity (assuming isotropic emission) of these sources for the velocity range ±8km.s-1 is egual to 1×1047 ph.s-1 and 2×1049 ph.s-1 respectively. The time behaviour of the water maser source in W49N during more than 7yr is monitored for the first time.

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Models of circumstellar molecular radio line emission

Astronomy and Astrophysics ◽

10.1051/0004-6361:20010072 ◽

2001 ◽

Vol 368 (3) ◽

pp. 969-993 ◽

Cited By ~ 142

Author(s):

F. L. Schöier ◽

H. Olofsson

Keyword(s):

Line Emission ◽

Radio Line

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The Kinematics of the Ionized Filaments in Sgr A West

Symposium - International Astronomical Union ◽

10.1017/s0074180900186863 ◽

1989 ◽

Vol 136 ◽

pp. 437-441 ◽

Cited By ~ 1

Author(s):

E. Serabyn

Keyword(s):

Orbital Motion ◽

Line Emission ◽

Ionized Gas ◽

Radio Line ◽

Kinematic Models ◽

Sgr A

The ionized gas within a few parsecs of the center of our galaxy is contained primarily in a number of thin elongated filaments (Ekers, this volume). Infrared and radio line observations have succeeded in determining the gas velocities along the majority of these filaments. A comparison of the line emission velocities with general kinematic models indicates that the motion of the filaments between 0.3 and 2 pc from the center is consistent with predominantly orbital motion.

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

International Astronomical Union Colloquium ◽

10.1017/s0252921100026002 ◽

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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Iron K-Line Emission from X-Ray Binaries

International Astronomical Union Colloquium ◽

10.1017/s0252921100107389 ◽

1988 ◽

Vol 102 ◽

pp. 47-50

Author(s):

K. Masai ◽

S. Hayakawa ◽

F. Nagase

Keyword(s):

Accretion Disk ◽

Radiative Recombination ◽

Characteristic Temperature ◽

Line Emission ◽

Ionization Front ◽

Continuum Radiation ◽

X Ray ◽

Low Mass ◽

X Ray Binaries

AbstractEmission mechanisms of the iron Kα-lines in X-ray binaries are discussed in relation with the characteristic temperature Txof continuum radiation thereof. The 6.7 keV line is ascribed to radiative recombination followed by cascades in a corona of ∼ 100 eV formed above the accretion disk. This mechanism is attained for Tx≲ 10 keV as observed for low mass X-ray binaries. The 6.4 keV line observed for binary X-ray pulsars with Tx> 10 keV is likely due to fluorescence outside the He II ionization front.

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