2 edition of Mid infrared hydrogen recombination line emission from the maser star MWC 349A found in the catalog.
Mid infrared hydrogen recombination line emission from the maser star MWC 349A
1997 by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English
|Statement||Howard A. Smith ... [et al.].|
|Series||[NASA contractor report] -- NASA-112976., NASA contractor report -- NASA CR-112976.|
|Contributions||Smith, Howard A., United States. National Aeronautics and Space Administration.|
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Get this from a library. Mid infrared hydrogen recombination line emission from the maser star MWC A. [Howard A Smith; United States. National Aeronautics and Space Administration.;]. Far-infrared hydrogen recombination lines H15 alpha ( micrometers), H12 alpha ( micrometers), and H10 alpha ( micrometers) were detected in the peculiar luminous star MWC A.
Resolved radio emission from models of photoevaporated disks around massive young stars Line Emission from the Maser Star MWC A. resolved the mid-IR hydrogen recombination lines H6.
A 65 micron emission feature in star-forming regions -- Detection of a interstellar crystalline silicate feature. Mid-Infrared line diagnostics of active galaxies. A spectroscopic AGN survey with ISO-SWS: Hydrogen infrared recombination lines as a diagnostic tool for the geometry of the circumstellar material of hot stars: 05/ words-2 a rojas 31 degrees c dot center 17 high salinity 19 diabetic nephropathy 14 bcl x 14 color vision 16 mg ha 42 wood partridge 13 verticilla 3 12 8 alpha 13 haq di.
Orbits of Minor Planets (Bowell+ ) (astorb) MERLIN+VLA images of HDF/HFF sources (Muxlow+, ) The BAX Database (Blanchard+, ) (BAX,J/A+A//) Cataclysmic Binaries. word(s) sdev freq; rojas: abetimus: gii: chilensis: especies: Feb 15, · Sample records for xvi infrared stars UV, optical, and radio wavelength ranges.
To determine the viability of infrared (IR) hydrogen recombination lines as a magnetic diagnostic for these stars, we have obtained low-resolution dramatic changes in the Be star emission line profiles are also seen during X-ray outbursts. On the left, the n91 → n90 (H90α) hydrogen line observations from Pushchino.
a The spectrogram toward the Omega nebula. b The test spectrogram with the antenna oﬀ the source. c The average of seven spectra toward Omega and the ﬁve test spectra made in April The abscissa is frequency; the ordinate, the antenna temperature. The disk-like component is elongated along PA ~ 46° and oriented perpendicular to the ionisation cone and outflow.
The extended component is responsible for 80% of the mid-infrared emission. It is elongated along PA ~ °, which is roughly perpendicular to the disk component and thus in polar direction.
Authors: Gemma Busquet (1), Robert Estalella (1), Qizhou Zhang (2), Serena Viti (3), Aina Palau (4), Paul T.P. Ho (2,5), Alvaro Sanchez-Monge (1) ((1) Departamentd. High Time Resolution Astrophysics - D.
Phelan, O. Ryan, A. Shearer - Free ebook download as PDF File .pdf), Text File .txt) or read book online for free.
High Time Resolution Astrophysics (HTRA) is an important new window to the universe and a vital tool in understanding a range of phenomena from diverse objects and radiative processes. The optical emission line variations were observed to be correlated with the optical continuum , and the emission line flares were found to exhibit a double-peaked line High-Speed Optical Observations of X-ray Binaries 43 profile, suggestive of emission distributed across the accretion disk rather than arising in localized regions.