In-flight performance of the IUE

Boggess, A.; Bohlin, R. C.; Evans, D. C.; Freeman, H. R.; Gull, Theodore R.; Heap, S. R.; Klinglesmith, Daniel A.; Longanecker, G. R.; Sparks, W. M.; West, D. K.; Holm, A. V.; Perry, P. M.; Schiffer, F. H.; Turnrose, B. E.; Wu, Chi-Chao; Lane, A. L.; Linsky, J. L.; Savage, Blair D.; Benvenuti, P.; Cassatella, A.; Clavel, J.; Heck, André; Macchetto, F.; Penston, M. V.; Selvelli, P. L.; Dunford, E.; Gondhalekar, P. M.; Oliver, Muellenhoff; Sandford, M. C. W.; Stickland, D. J.; Boksenberg, A.; Coleman, C. I.; Snijders, M. A. J.; Wilson, R.

doi:10.1038/275377a0

Cited by 92 publications

(15 citation statements)

References 9 publications

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“…We have examined the IUE database for the sources in our survey and find that only three objects in our survey sample were observed: R LMi, V Hya, and TW Hor. R LMi and TW Hor were observed with both the long-wavelength (LWR and LWP) and short-wavelength (SWP) instruments (Boggess et al 1978a(Boggess et al , 1978b, whereas V Hya was observed only with the long-wavelength instrument. For both R Lmi and V Hya, the signal-to-noise ratio (S/ N ) over the observed bandpasses (1910 Y3300 8 for LWR/LWP and 1150 Y 1975 8 for the SWP) is close to zero.…”

Section: Ultraviolet Excessesmentioning

confidence: 97%

Binarity in Cool Asymptotic Giant Branch Stars: AGALEXSearch for Ultraviolet Excesses

Sahai

Findeisen

Paz

et al. 2008

Astrophysical Journal

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The search for binarity in AGB stars is of critical importance for our understanding of how planetary nebulae acquire the dazzling variety of aspherical shapes which characterizes this class. However, detecting binary companions in such stars has been severely hampered due to their extreme luminosities and pulsations. We have carried out a small imaging survey of AGB stars in ultraviolet light (using GALEX ), where these cool objects are very faint, in order to search for hotter companions. We report the discovery of significant far-ultraviolet excesses toward nine of these stars. The far-ultraviolet excess most likely results either directly from the presence of a hot binary companion or indirectly from a hot accretion disk around the companion.

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Section: Ultraviolet Excessesmentioning

confidence: 97%

Binarity in Cool Asymptotic Giant Branch Stars: AGALEXSearch for Ultraviolet Excesses

Sahai

Findeisen

Paz

et al. 2008

Astrophysical Journal

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“…The primary data used in our analysis are NEWSIPS lowdispersion IUE UV spectra (Boggess et al 1978a(Boggess et al , 1978bNichols & Linsky 1996), corrected and placed on the HST -FOS system (Bohlin 1996) using the algorithms developed by MF99. Data from both the long wavelength (LWR and LWP) and short wavelength (SWP) cameras are required and the wavelength regions covered are 1978-3000 Å and 1150-1978 Å, respectively.…”

Section: The Datamentioning

confidence: 99%

Determining the Physical Properties of the B Stars. I. Methodology and First Results

Fitzpatrick

Massa

1999

ApJ

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We describe a new approach to Ðtting the UV-to-optical spectra of B stars to model atmospheres and present initial results. Using a sample of lightly reddened stars, we demonstrate that the Kurucz model atmospheres can produce excellent Ðts to either combined low-dispersion IUE and optical photometry or HST FOS spectrophotometry, as long as the following conditions are fulÐlled : (1) an extended grid of Kurucz models is employed ; (2) the IUE NEWSIPS data are placed on the FOS absolute Ñux system using the Massa & Fitzpatrick transformation ; (3) and all of the model parameters and the e †ects of interstellar extinction are solved for simultaneously. When these steps are taken, the temperatures, gravities, abundances, and microturbulence velocities of lightly reddened B0ÈA0 V stars are determined to high precision. We also demonstrate that the same procedure can be used to Ðt the energy distributions of stars that are reddened by any UV extinction curve that can be expressed by the Fitzpatrick & Massa parameterization scheme. We present an initial set of results and verify our approach through comparisons with angular diameter measurements and the parameters derived for an eclipsing B-star binary. We demonstrate that the metallicity derived from the ATLAS9 Ðts to main-sequence B stars is essentially the Fe abundance. We Ðnd that a near zero microturbulence velocity provides the best Ðt to all but the hottest or most luminous stars (where it may become a surrogate for atmospheric expansion) and that the use of white dwarfs to calibrate UV spectrophotometry is valid.

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“…Although there were a few limited observations of the UV spectra of F-M dwarf stars with spectrographs on sounding rockets and the Copernicus spacecraft, the International Ultraviolet Explorer (IUE) [32] obtained the first large sample of spectra for the stars covering the full UV spectral range during its 18-year mission. IUE obtained spectra over the range 115-330 nm with both moderate (13,000-17,000) or low (280-430) resolving power (∆λ/λ).…”

Section: Stellar Ultraviolet Spectramentioning

confidence: 99%

The Radiation Environment of Exoplanet Atmospheres

Linsky

2014

Challenges

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Exoplanets are born and evolve in the radiation and particle environment created by their host star. The host star's optical and infrared radiation heats the exoplanet's lower atmosphere and surface, while the ultraviolet, extreme ultraviolet and X-radiation control the photochemistry and mass loss from the exoplanet's upper atmosphere. Stellar radiation, especially at the shorter wavelengths, changes dramatically as a host star evolves leading to changes in the planet's atmosphere and habitability. This paper reviews the present state of our knowledge concerning the time-dependent radiation emitted by stars with convective zones, that is stars with spectral types F, G, K, and M, which comprise nearly all of the host stars of detected exoplanets.

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In-flight performance of the IUE

Cited by 92 publications

References 9 publications

Binarity in Cool Asymptotic Giant Branch Stars: AGALEXSearch for Ultraviolet Excesses

Binarity in Cool Asymptotic Giant Branch Stars: AGALEXSearch for Ultraviolet Excesses

Determining the Physical Properties of the B Stars. I. Methodology and First Results

The Radiation Environment of Exoplanet Atmospheres

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