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2 edition of The evolution of ultraviolet emission lines from circumstellar material surroundings SN 1987A found in the catalog.

The evolution of ultraviolet emission lines from circumstellar material surroundings SN 1987A

The evolution of ultraviolet emission lines from circumstellar material surroundings SN 1987A

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Published by Stockholm Observatory, National Aeronautics and Space Administration, National Technical Information Service, distributor in Saltsjobaden, Sweden, [Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • Circumstellar matter.,
  • Supernovae.,
  • Ultraviolet spectra.

  • Edition Notes

    StatementGeorge Sonneborn ... [et al.].
    SeriesPreprint -- no. 82, NASA contractor report -- NASA CR-204193..
    ContributionsSonneborn, George., United States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL17127838M

    Stellar Spectroscopy The Message of Starlight Rev 3/9/04 Stellar Spectroscopy 1 as well as parts of the ultraviolet and infrared. The of the emission lines depend on the type of gas; e.g., Hydrogen gas produces different emission lines than Helium. Absorption lines can be best thought of as. Principal component analysis of two ultraviolet emission-lines pose the emission-lines into several independent components. Observational material All spectra were down-loaded from the uniform low dispersion archive (ULDA) version in the Swiss ULDA national host.

    Successful resolution of an ultraviolet divergence is known as ultraviolet completion. If they cannot be removed, they imply that the theory is not perturbatively well-defined at very short distances. The name comes from the earliest example of such a divergence, the "ultraviolet catastrophe" first encountered in understanding blackbody radiation. Sep 11,  · The emission spectrum of an unknown element contains two lines - one in the visible portion of the spectrum, and the other, ultraviolet. Based on the following figure and what you know about Niels Bohr's model of the atom, account for the difference in energy between these lines.

    Abstract: For supernova powered by the conversion of kinetic energy into radiation due to the interactions of the ejecta with a dense circumstellar shell, we show that there could be X-ray analogues of optically super-luminous SNe with comparable luminosities and energetics. We consider X-ray emission from the forward shock of SNe ejecta colliding into an optically-thin CSM shell, derive Cited by: Astronomers have developed a way to detect the ultraviolet (UV) background of the Universe, which could help explain why there are so few small galaxies in the cosmos.


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The evolution of ultraviolet emission lines from circumstellar material surroundings SN 1987A Download PDF EPUB FB2

SN A was a type II supernova in the Large Magellanic Cloud, a dwarf galaxy satellite of the Milky ogmaexpo.com occurred approximately kiloparsecs (, light-years) from Earth and was the closest observed supernova since Kepler's Supernova. A's light reached Earth on February 23,and as the earliest supernova discovered that year, was labeled "A".Date: February 24, ( UTC), Las Campanas.

Abstract. Discovery in of narrow emission lines in the ultraviolet spectrum of SN A (WAMSTEKER et al. [1]) provided the first direct evidence for Author: George Sonneborn. The three bright rings around SN A that were visible after a few months in images by the Hubble Space Telescope are material from the stellar wind of the progenitor.

These rings were ionized by the ultraviolet flash from the supernova explosion, and consequently began emitting in various emission lines. Physical Conditions in Circumstellar Gas surrounding SN A 12 Years After Outburst.

The UV emission lines of the inner ring rev ealed that the SN A circumstellar material. Optical and Ultraviolet Spectroscopy of SN N: Evidence for Strong Circumstellar Interaction Article in The Astrophysical Journal (1) · August with 7 Reads How we measure 'reads'.

SN A was a type II supernova in the Large Magellanic Cloud, a dwarf galaxy satellite of the Milky ogmaexpo.com occurred approximately kiloparsecs (, light-years) from Earth and was the closest observed supernova since Kepler's Supernova, visible from earth in A's light reached Earth on February 23,and as the earliest supernova discovered that year, was labeled "A".Date: February 24, ( UTC), Las Campanas.

Ultraviolet Emission Lines from Circumstellar Gas Surrounding SN A.- Asymmetry in the Wind from the Precursor to SN A.- Comments on the IR Emission from the Subarcsec Vicinity of SN A.- A Third, Inner Light Echo Ring Around SN A.- Nimba Around Supernova A: Kinematics and Evolution in Ages.- Circumstellar and Interstellar.

Far-Ultraviolet H 2 Emission from Circumstellar Disks: Authors: the fact that the non-accreting sources show no H 2 emission implies that the H 2 gas in the inner disk has dissipated in the non-accreting sources, although dust (and possibly gas) remains at larger radii.

We hypothesize that this emission originates above the photosphere, and is related to interaction with circumstellar material (CSM) located in close proximity to the SN progenitor.

In contrast, the spectra of SN ig are well fit by single-temperature models, display weak continuum and strong reverse-fluorescence features, and are similar to Cited by: SN A was a supernova in the outskirts of the Tarantula Nebula in the Large Magellanic Cloud, a nearby dwarf galaxy.

It occurred approximately kiloparsecs from Earth, [1] close enough that it was visible to the naked eye.

It could be seen from the Southern Hemisphere. It was the closest observed supernova since SN Constellation: Dorado. Interior, the innermost circumstellar material lies along a cylindrical hourglass, 1 ly in radius and 4 ly long, which connects to the peanut by a thick equatorial disk. The nebulae are inclined 41o south and 8o east of the line of sight, slightly elliptical in cross section, and marginally offset west of the ogmaexpo.com by: Using International Ultraviolet Explorer (IUE) spectra of previously studied giants together with our HST spectra, we investigate whether the chromospheric and transition layer emission-line spectra of the Ba stars are different from those of nonpeculiar giants and from those of giants with peculiar carbon and/or nitrogen abundances.

Start studying Chapter 4: Light and Atoms. Learn vocabulary, terms, and more with flashcards, games, and other study tools. The different emission sites (ionised but unshocked ring material, shocked ring gas, reverse shock, inner supernova ejecta) account for the vastly different velocities, and are easily separated in the Figure 1.

Left: combined HST (green), Chandra (blue) and ALMA (red) image of SN A. Right: NACO data taken in January in the Ks-band. Identifying Emission Lines in the Solar Extreme Ultraviolet (EUV) Irradiance Spectrum Rachael L.

Tomasino Advisors: Dr. Frank Eparvier and Rachel Hock University of Colorado, Boulder Laboratory for Atmospheric and Space Physics August 4, Exploring a principal means of understanding the Sun's atmosphere, its ultraviolet and soft X-ray emission, this book includes a list of emission lines in the ultraviolet and soft X-ray region, and a glossary of terms.

An ideal reference for graduate students and researchers in Cited by: Exploring a principal means of understanding the Sun's atmosphere, its ultraviolet and soft X-ray emission, this book includes a list of emission lines in the ultraviolet and soft X-ray region, and a glossary of terms.

An ideal reference for graduate students and researchers in astrophysics and solar ogmaexpo.com: Kenneth J. Phillips. Recently, however, Ödeen et al.

argued that the evolution of ultraviolet sensitive vision in Passeriformes is more complex than a single VS to UVS opsin shift in an ancestor of Passerida, presenting molecular evidence for additional UV shifts from VS colour vision outside Passerida, in fairywrens, genus Supplementary ogmaexpo.com by: Jul 29,  · (, July 29).

Discovery of new emission lines from highly charged heavy ions: Constructing an experimental database of extreme ultraviolet spectra. ScienceDaily. Retrieved December 16. Extreme ultraviolet emission and confinement of tin plasmas in the presence of a magnetic field Amitava Roy,1,2,a) Syed Murtaza Hassan,1 Sivanandan S.

Harilal,1 Akira Endo,2 Tomas Mocek,2 and Ahmed Hassanein1 1School of Nuclear Engineering and Center for Materials Under Extreme Environment(CMUXE), Purdue University, West Lafayette, IndianaUSA.

Ultraviolet radiation is known to inhibit photosynthesis, induce DNA destruction and cause damage to a wide variety of proteins and lipids. In particular, UV radiation between and nm becomes energetically very damaging to most of the terrestrial biological ogmaexpo.com by: THE EVOLUTION OF FAR-UV AND NEAR-UV EMISSION FROM EARLY M STARS Online-only material: color figures 1.

INTRODUCTION The conditions inside the circumstellar disks of M dwarfs by strong emission lines (Civ,Cii,Siiv,Heii) originating .Assignment 3. STUDY. Flashcards. Learn. Write. Spell. Test. PLAY. Match. Gravity. Created by. Emission of visible light by a material when it's exposed to ultraviolet radiation.

Ultraviolet (UV) Light wavelength that's invisible to the human eye. Fancy-colored diamonds (Fancies) Naturally colored yellow and brown diamonds that exhibit color.