The Evolution of Ultraviolet Emission Lines From Circumstellar Material Surrounding SN 1987A

AbstractMass loss from the B3 Ia progenitor star for SN 1987A is revealed by the recent emergence of narrow ultraviolet emission lines. The emitting gas is nitrogen-rich, has low velocity, and may be located a light-year from the supernova. This gives every sign of having been ejected from the SK −69 202 progenitor when it was a red supergiant, prior to its brief and ultimately violent life as a blue supergiant. Changes in the hydrogen line profiles during the early evolution provide a way to estimate the density distribution in the supernova atmosphere, and the mass of hydrogen it contains. A preliminary estimate is that the power-law index of density in the envelope goes as V−11 and the mass that lies above a velocity of 6, 000 km s−1 is between 1 and 6 solar masses.

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Narrow ultraviolet emission lines from SN 1987A - Evidence for CNO processing in the progenitor

The Astrophysical Journal ◽

10.1086/167022 ◽

1989 ◽

Vol 336 ◽

pp. 429 ◽

Cited By ~ 133

Author(s):

C. Fransson ◽

A. Cassatella ◽

R. Gilmozzi ◽

R. P. Kirshner ◽

N. Panagia ◽

...

Keyword(s):

Emission Lines ◽

Ultraviolet Emission ◽

Sn 1987A

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Solar abundance determination from ultraviolet emission lines

Solar Physics ◽

10.1007/bf00150858 ◽

1967 ◽

Vol 1 (2) ◽

pp. 229-241 ◽

Cited By ~ 66

Author(s):

Andrea K. Dupree ◽

Leo Goldberg

Keyword(s):

Emission Lines ◽

Solar Abundance ◽

Ultraviolet Emission ◽

Abundance Determination

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Interpretation of the Ultraviolet Spectrum of NGC 7662

Symposium - International Astronomical Union ◽

10.1017/s0074180900142676 ◽

1978 ◽

Vol 76 ◽

pp. 121-122

Author(s):

R.C. Bohlin ◽

J.P. Harrington ◽

T.P. Stecher

Keyword(s):

Neutral Hydrogen ◽

Central Star ◽

Dielectronic Recombination ◽

Emission Lines ◽

Ultraviolet Emission ◽

Two Photon ◽

Carbon Abundance ◽

Photon Process ◽

Ngc 7662

The ultraviolet emission lines that were me asured in the spectrum obtained from our rocket observation of NGC 7662 have been compared with those predicted by a set of models. The models allow a determination of the carbon abundance which is found to be solar and the C/0 ratio which is equal to unity. In order to obtain a good fit, dielectronic recombination and charge exchange between neutral hydrogen and C IV were included, both of which increase the concentration of C III. The observed continuum consists of light from the central star and from the nebula, which contributed primarily via the two photon process in the H° and the Balmer continuum.

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CONSTRAINING UV CONTINUUM SLOPES OF ACTIVE GALACTIC NUCLEI WITH CLOUDY MODELS OF BROAD-LINE REGION EXTREME-ULTRAVIOLET EMISSION LINES

The Astrophysical Journal ◽

10.1088/0004-637x/793/2/100 ◽

2014 ◽

Vol 793 (2) ◽

pp. 100 ◽

Cited By ~ 7

Author(s):

Joshua Moloney ◽

J. Michael Shull

Keyword(s):

Active Galactic Nuclei ◽

Extreme Ultraviolet ◽

Galactic Nuclei ◽

Emission Lines ◽

Broad Line ◽

Ultraviolet Emission ◽

Broad Line Region ◽

Line Region

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Ultraviolet emission line imaging of planetary nebulae with GALEX

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312011167 ◽

2011 ◽

Vol 7 (S283) ◽

pp. 308-309 ◽

Cited By ~ 2

Author(s):

Luciana Bianchi ◽

Arturo Manchado ◽

Karl Forster

Keyword(s):

Galaxy Evolution ◽

Broad Band ◽

Planetary Nebulae ◽

Emission Lines ◽

Continuum Emission ◽

Ultraviolet Emission ◽

The Galaxy ◽

Optical Domain ◽

Line Imaging ◽

Shock Fronts

AbstractGALEX (the Galaxy Evolution Explorer) has provided far-UV(1344-1786Å) and near-UV(1771-2831Å) imaging of several Planetary Nebulae (e.g., Bianchi et al. 2008, Bianchi 2012), with flux limits ~27.5 mag/sq.arcsec for objects in the Medium-deph Imaging Survey (MIS). PNe images in the GALEX broad-band UV filters include flux from both nebular line and continuum emission. We use the GALEX grism observing mode to obtain slitless spectral imaging of a sample of PNe with diameters >1′, in the near-UV. We show the first data from this program. The grism produces 2D images of the prominent UV nebular emission lines, when such lines dominate the flux. Combined with monochromatic images of diagnostic lines in the optical domain, such data help detect and interpret ionization and shock fronts, especially in faint nebular regions.

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