Showing papers on "Blue dwarf published in 1978"
10 citations
9 citations
8 citations
1 May 1978
TL;DR: The dwarf-nova phenomenon could result from a local accumulation of hydrogen being accreted onto the surface of a degenerate dwarf near its magnetic poles, which would produce a flare as mentioned in this paper.
Abstract: The dwarf-nova phenomenon could result from a local accumulation of hydrogen being accreted onto the surface of a degenerate dwarf near its magnetic poles Thermonuclear buring in this hydrogen layer would produce a flare A magnetic field of (3--30) x 10/sup 6/ gauss is needed to guide the accretion The origin of the optical and x-ray emission of dwarf novae is discussed
6 citations
Journal Article•
4 citations
TL;DR: A white dwarf is a body of stellar mass, but of planetary dimensions, which is self luminous with a surface temperature that has been observed as high as 70,000 K or as low as 4, 000 K as discussed by the authors.
Abstract: A white dwarf is a body of stellar mass, but of planetary dimensions. It is self luminous with a surface temperature that has been observed as high as 70,000 K or as low as 4,000 K. Because of its low surface area the star is far fainter than a main sequence star of the same colour; equally the light it emits is bluer than that from a main sequence star of similar luminosity. Figure 1 is the HR diagram from data obtained by the US Naval Observatory showing the dwarf and white dwarf sequences.
3 citations
TL;DR: An emission-line blue star of small proper motion, GD 552, has been found among the suspected white dwarfs of the Lowell lists as discussed by the authors, which has a nearly flat continuum and strong Balmer emission lines, about 2000 km/s in width.
Abstract: An emission-line blue star of small proper motion, GD 552, has been found among the suspected white dwarfs of the Lowell lists. It has a nearly flat continuum and strong Balmer emission lines, about 2000 km/s in width. Lowell photographs do not show any large variability, yet its spectrum resembles that of an old nova or U Gem star. It is interpreted as a white dwarf with a weak accretion disk, each contributing about one-half the light. Its absolute magnitude is about + 13, considerably fainter than the normally accepted value for U Gem stars.