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Title: Ultraviolet observations of LMC nova 1988

Abstract

This current bright novae was first detected in outburst on March 21, 1988. Its discovery has given us the opportunity of studying the first extragalactic nova in the ultraviolet and we have, therefore, obtained a number of LWP and SWP spectra when it was at maximum. We have also obtained a high dispersion LWP spectrum in order to study the ISM in the Large Magellanic Cloud on a slightly different line-of-sight from that analyzed using SN 1987A. 10 refs., 2 figs.

Authors:
; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ;
Publication Date:
Research Org.:
Los Alamos National Lab., NM (USA)
OSTI Identifier:
6921466
Report Number(s):
CONF-8806226-1
ON: DE88016319
DOE Contract Number:
W-7405-ENG-36
Resource Type:
Conference
Resource Relation:
Conference: Conference on a decade of UV astronomy with the IUE satellite, Washington, DC, USA, 1 Jun 1988; Other Information: Portions of this document are illegible in microfiche products
Country of Publication:
United States
Language:
English
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; NOVAE; ULTRAVIOLET SPECTRA; MAGELLANIC CLOUDS; ULTRAVIOLET RADIATION; ELECTROMAGNETIC RADIATION; ERUPTIVE VARIABLE STARS; GALAXIES; RADIATIONS; SPECTRA; STARS; VARIABLE STARS 640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar, Radio & X-Ray Sources

Citation Formats

Starrfield, S., Stryker, L.L., Sonneborn, G., Sparks, W.M., Sion, E.M., Wagner, R.M., Ferland, G., Gallagher, J.S., Wade, R., Williams, R.E., Heathcote, S., Kenyon, S., Shaviv, G., Wehrse, R., Hauschildt, P., Truran, J.W., Wu, C.C., Gehrz, R.D., and Ney, E.P. Ultraviolet observations of LMC nova 1988. United States: N. p., 1988. Web.
Starrfield, S., Stryker, L.L., Sonneborn, G., Sparks, W.M., Sion, E.M., Wagner, R.M., Ferland, G., Gallagher, J.S., Wade, R., Williams, R.E., Heathcote, S., Kenyon, S., Shaviv, G., Wehrse, R., Hauschildt, P., Truran, J.W., Wu, C.C., Gehrz, R.D., & Ney, E.P. Ultraviolet observations of LMC nova 1988. United States.
Starrfield, S., Stryker, L.L., Sonneborn, G., Sparks, W.M., Sion, E.M., Wagner, R.M., Ferland, G., Gallagher, J.S., Wade, R., Williams, R.E., Heathcote, S., Kenyon, S., Shaviv, G., Wehrse, R., Hauschildt, P., Truran, J.W., Wu, C.C., Gehrz, R.D., and Ney, E.P. 1988. "Ultraviolet observations of LMC nova 1988". United States. doi:.
@article{osti_6921466,
title = {Ultraviolet observations of LMC nova 1988},
author = {Starrfield, S. and Stryker, L.L. and Sonneborn, G. and Sparks, W.M. and Sion, E.M. and Wagner, R.M. and Ferland, G. and Gallagher, J.S. and Wade, R. and Williams, R.E. and Heathcote, S. and Kenyon, S. and Shaviv, G. and Wehrse, R. and Hauschildt, P. and Truran, J.W. and Wu, C.C. and Gehrz, R.D. and Ney, E.P.},
abstractNote = {This current bright novae was first detected in outburst on March 21, 1988. Its discovery has given us the opportunity of studying the first extragalactic nova in the ultraviolet and we have, therefore, obtained a number of LWP and SWP spectra when it was at maximum. We have also obtained a high dispersion LWP spectrum in order to study the ISM in the Large Magellanic Cloud on a slightly different line-of-sight from that analyzed using SN 1987A. 10 refs., 2 figs.},
doi = {},
journal = {},
number = ,
volume = ,
place = {United States},
year = 1988,
month = 1
}

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  • We present a brief summary of the outburst for a nova that was discovered in November 1987 and has been followed since that time. Although we were able to observe it with the IUE at maximum, its ultraviolet energy faded rapidly and after the first two weeks we were no longer able to observe it at IUE wavelengths. It was observed to form a thick dust shell and currently is in the nebular stage. 6 figs.
  • Nova Vul 1984 /number sign/2 has been observed with the IUE Satellite from December 1984 through November 1987 and we expect to be able to observe it with the IUE Satellite for at least another two years. These spectra are characterized by strong lines from Mg, Ne, C, Si, O, N, and other elements. Data obtained in the ultraviolet, infrared, and optical show that this nova is ejecting material rich in oxygen, neon, and magnesium. 16 refs., 5 figs., 1 tab.
  • Two XMM-Newton observations of the fast classical nova V2491 Cyg were carried out in short succession on days 39.93 and 49.62 after discovery, during the supersoft source (SSS) phase, yielding simultaneous X-ray and UV light curves and high-resolution X-ray spectra. The first X-ray light curve is highly variable, showing oscillations with a period of 37.2 minutes after an extended factor of three decline lasting {approx}3 hr, while the second X-ray light curve is less variable. The cause of the dip is currently unexplained and has most likely the same origin as similar events in the early SSS light curves ofmore » the novae V4743 Sgr and RS Oph, as it occurred on the same timescale. The oscillations are not present during the dip minimum and also not in the second observation. The UV light curves are variable but contain no dips and no period. High-resolution X-ray spectra are presented for four intervals of differing intensity. All spectra are atmospheric continua with deep absorption lines and absorption edges. Two interstellar lines of O I and N I are clearly seen at their rest wavelengths, while a large number of high-ionization absorption lines are found at blueshifts indicating an expansion velocity of 3000-3400 km s{sup -1}, which does not change significantly during the epochs of observation. Comparisons with the slower nova V4743 Sgr and the symbiotic recurrent nova RS Oph are presented. The SSS spectrum of V4743 Sgr is much softer with broader and more complex photospheric absorption lines. The ejecta are extended, allowing us to view a larger range of the radial velocity profile. Meanwhile, the absorption lines in RS Oph are as narrow as in V2491 Cyg, but they are less blueshifted. A remarkable similarity in the continua of V2491 Cyg and RS Oph is found. The only differences are smaller line shifts and additional emission lines in RS Oph that are related to the presence of a dense stellar wind from the evolved companion. Three unidentified absorption lines are present in the X-ray spectra of all three novae, with projected rest wavelengths 26.05 A, 29.45 A, and 30.0 A. No entirely satisfactory spectral model is currently available for the soft X-ray spectra of novae in outburst, and careful discussion of assumptions is required.« less
  • The conference presents papers on the chemical analysis of UV rocket plume signatures, the determination of daytime midlatitude electron density profiles from satellite UV and in-situ data, and the application of CCD detectors to UV imaging from a spinning satellite. Other topics include a middle atmosphere high-resolution spectrograph, very large format pulse-counting UV detectors, optical filters for high-resolution UV imaging systems, and synthetic dayglow spectra and the Rayleigh scattering background from the FUV to the visible. Consideration is also given to image motion compensation using a photon-counting UV/visible detector, UV/ozone removal of contaminants in spacecraft environments, and decoding techniques formore » fine-fine geometry multianode microchannel arrays.« less
  • Various papers on X-ray and vacuum ultraviolet interaction data bases, calculations, and measurements are presented. Individual topics addressed include: photoabsorption and photoionization cross sections, a program to obtain reliable photoabsorption cross sections, photoionization of small molecules using synchrotron radiation, components of the photoionization cross section in the VUV and soft X-ray region, photoabsorption and fluorescence cross sections of halogen compounds in VUV, near-threshold X-ray fluorescence spectroscopy of molecules, atomic processes in tokamak plasmas, and photoionization studies of atomic oxygen and nitrogen. Also considered are: constraints and data base of X-ray optical properties, theory of anomalous X-ray scattering from atoms andmore » ions, preparation of multilayered X-ray photoabsorption targets, composition and thickness of multilayer foils using MeV ion-beam techniques, recent developments with VUV and soft X-ray detector systems, and measurements of X-ray fluorescence yields of plastics by photoexcitation.« less