Zobrazeno 1 - 10
of 28
pro vyhledávání: '"Irene R. Little-Marenin"'
Autor:
Irene R. Little-Marenin
Publikováno v:
Symposium - International Astronomical Union. 177:361-366
The circumstellar shells of M stars produce emission features due to amorphous silicates peaking around 10 and 18 μm, with additional emission at 11 μm due to crystalline olivine and at 13.1 μm (unknown carrier). C stars are associated with SiC du
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::592c1917e838e959c20ccf51a4c587cc
https://doi.org/10.1017/s0074180900002606
https://doi.org/10.1017/s0074180900002606
Publikováno v:
The Astronomical Journal. 115:809-820
We have developed a classification system for the infrared spectral emission from carbon stars, using a sample of 96 bright carbon-rich variables associated with the asymptotic giant branch. In addition to the stellar contribution, most spectra inclu
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::b0acd414e938d8b77b77f824f506a566
https://doi.org/10.1086/300205
https://doi.org/10.1086/300205
Publikováno v:
Cool Stars, Stellar Systems, and the Sun ISBN: 9783540186533
We observe a progression of emission features in the 8–11 μm region in MS, S and SC stars that parallels their increasing C:O ratio and s-process enhancements.
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::97961819b72eaab7f16925dab4f12444
https://doi.org/10.1007/3-540-18653-0_159
https://doi.org/10.1007/3-540-18653-0_159
Publikováno v:
Cool Stars, Stellar Systems, and the Sun ISBN: 9783540186533
We observed the 22.2 GHz H2O maser line from the two C stars EU And and V778 Cyg. The intensity of the line has varied by more than a factor of 5 over several month and the line has shown additional weaker components. We interpret the system as being
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::600944f9ff19d79e0db63dd11435dd7d
https://doi.org/10.1007/3-540-18653-0_165
https://doi.org/10.1007/3-540-18653-0_165
Publikováno v:
Cool Stars, Stellar Systems, and the Sun ISBN: 9783540167631
The Infrared Astronomical Satellite (IRAS) carried a low resolution spectrometer (LRS) with a wavelength response covering the 8 to 22 micrometer region. About 5000 LRS spectra exist of point sources brighter than 10 Jy at 12 and 25 micrometers. Spec
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::ac42f01f41bd3cb034e98df99f33c44e
https://doi.org/10.1007/3-540-16763-3_227
https://doi.org/10.1007/3-540-16763-3_227
Publikováno v:
Cool Stars, Stellar Systems, and the Sun ISBN: 9783540167631
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::58d86cee53cbc8643577a2a4713b6351
https://doi.org/10.1007/3-540-16763-3_226
https://doi.org/10.1007/3-540-16763-3_226
Publikováno v:
ESO Astrophysics Symposia ISBN: 9783662113929
We observed the 22 GHz water maser emission in VX UMa (M8e, M=388 d ) and V778 Cyg (C5,5J, SRb=300 d ) from 1987-1992. The spectra of both stars show three distinct components. All three components vary periodically in intensity. We interpret these f
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::c652a3627ebfa6ed41e82748dc7ee815
https://doi.org/10.1007/978-3-540-68597-5_16
https://doi.org/10.1007/978-3-540-68597-5_16
Autor:
Irene R. Little-Marenin
Publikováno v:
ESO Astrophysics Symposia ISBN: 9783662113929
Mira variables pulsate with periods ranging from 100–2000 days and eject copious quantities of gas into space. Part of the gas condenses into dust grains when T < 1200 K in the shell. During their pulsational cycle Miras vary in luminosity, forcing
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::57a5257574bfb98ad0afce7e0c3a8b1d
https://doi.org/10.1007/978-3-540-68597-5_15
https://doi.org/10.1007/978-3-540-68597-5_15
Publikováno v:
Astrophysical Masers ISBN: 9783540563433
We have monitored the 22 GHz H2O maser line from 22 LPVs since 1987. All stars show highly variable water maser emission with most Miras having a phase lag of 0.3 phase between the water maser and optical emission. VX UMa appears to show variations a
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::092d797c7899893ace726133f51b1a34
https://doi.org/10.1007/3-540-56343-1_259
https://doi.org/10.1007/3-540-56343-1_259
Publikováno v:
Astrophysical Masers ISBN: 9783540563433
The water maser spectra of V778 Cyg show periodic variations with the same period as the optical carbon star (P=302d). However, a phaselag of 0.23 is present. The central velocity of the features may show long term variability. The 22 GHz spectra of
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_________::056bbfe2e71eff5413bb0c1afaf5c7fc
https://doi.org/10.1007/3-540-56343-1_265
https://doi.org/10.1007/3-540-56343-1_265