«LATE-TYPE STAR» 관련 영어 책
다음 도서 목록 항목에서
late-type star 의 용법을 확인하세요.
late-type star 에 관련된 책과 해당 책의 짧은 발췌문을 통해 영어 서적에서 단어가 사용되는 맥락을 제공합니다.
1
Cataclysmic Variables and Related Objects
Paczynski and Sienkiewicz (l98l), and Rappaport, Joss, and Webbink (l982) have
provided a theoretical explanation of the minimum period that appears to be at
least qualitatively correct. The mass of the late type star in a cataclysmic variable
...
International Astronomical Union. Colloquium, Mario Livio, G. Shaviv, 1983
2
Imaging of
Late-
type Stars Using Mid-infrared Interferometry
3.3 Late-Type Stars The name late-type star hails from the days when large cool
stars were all thought to be representative of the late stages of stellar evolution
and the hot luminous stars were younger stages of stars on the main sequence.
3
Planetary Nebulae: Observations and Theory
26 +1.1 V-V 1-8 Very probably an HI I region (Chopinet, Lortet- Zuckermann,
1976). 44 +8.1 K 3-10 Resembling late-type star (Class S) (Allen 1974). Not a PN
, MS star (Allen, Fosbury, 1975). 45 -0.1 K 4-21 Resembling late-type star (Class
S) ...
4
Cataclysmic Variables and Related Objects: Proceedings of ...
The fraction of light from the late type star in the non-eclipsing nova-like variable
IX Vel (Haug 1988) in the A'-band is about 20. . .40%, in agreement with WY Sge.
At K maximum light occurs at phase 0.32 ±0.01 which implies that the out of ...
International Astronomical Union. Colloquium, A. Evans, Janet H. Wood, 1996
5
A Dictionary of Astronomy
See also HUBBLE CLASSIFICATION. late-type star A star with a surface
temperature cooler than the Sun, with a spectral type K, M, C, or S; G stars are
often included as well. Late-type stars can be either of low mass, if they are on
the main ...
6
Extreme Ultraviolet Astronomy
The peak distance for white dwarfs lies at 60–80 pc, while most late-type star
classes have maxima at ≈20 pc. G stars appear to be visible out to greater
distances (50 pc) probably because of the population of RS CVn binaries, which
are ...
Martin A. Barstow, Jay B. Holberg, 2003
7
Frontiers of Astrophysics
It could be that the central star has reached a highly evolved state, i.e., is a late-
type star, and is losing mass. The dust shell is the condensate of the mass
ejected by the star. An alternative interpretation is that the central star is an early-
type ...
8
Spectroscopic Astrophysics: An Assessment of the ...
... of combination of a late-type star and an early-type companion — which, in this
case, is nova-like — is by no means exceptional. Several other objects of the
same type have recently been investigated, namely, T Coronae Borealis8 (nova
+ ...
They are — stellar objects, — show emission from ions with IP > 55 eV, i.e. Hell,
— show evidence for G or later spectral type, — if no evidence for late-type star,
then lines with IP > 100 eV must be present, i.e. e.g. [FeVll]. The model invoked to
...
Anne Marie Hubert, Carlos Jaschek, 1998
10
Formation and Evolution of Galaxy Bulges (IAU S245)
For these galaxies, we use the photometric' UBVRIK SED to select late-type star-
forming galaxies. 2) The redshift of the galaxy places Ha (or [OIIIJ5007 for z > 1.8
galaxies) emission line between the OH sky lines in the H or K bands. 3) The ...
International Astronomical Union. Symposium, Martin Bureau, E. Athanassoula, 2008
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Hubble's 1923 Nova in Andromeda Erupts Again!
They are semi-detached binary systems where an evolved, late-type star fills its Roche lobe and transfers mass to its white dwarf companion. «Universe Today, 2월 12»
