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Subluminous Stars in the HR Diagram

  • C. C. Dahn (a1) and R. S. Harrington (a1)

Extract

Eggen (1969) has defined a subluminous star “… as one that is fainter by at least a factor of 10 in visual luminosity than the main sequence stars of the same(U-V).” Implicit is the suggestion that single stars might exist in the region of the HR diagram between the subdwarfs and the normal degenerate sequence. While the evolutionary calculations of Chin and Stothers (1971) indicate that stars with masses <0.2 M will pass through this region following the completion of nuclear burning, these models have not yet been confirmed. We summarize Naval Observatory astrometry and photometry as it pertains to the existence of such stars.

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Copyright

References

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Chin, C. and Stothers, R. (1971). Astrophys. J. 163, 555.
Eggen, O. J. (1969). Astrophys. J. 157, 287.
Eggen, O. J. (1970). Astrophys. J. 159, 945.
Eggen, O. J. (1971). In IAU Symposium No. 42, White Dwarfs. Luyten, W.J., ed., D. Reidel, Dordrecht, p. 8.
Luyten, W. J. (1957). A Catalogue of 9867 Stars in the Southern Hemisphere with Proper Motions Exceeding 0″2 Annually, Lund Press, Minneapolis.
van Altena, W. F. (1969). Astron. J. 74, 2.

Subluminous Stars in the HR Diagram

  • C. C. Dahn (a1) and R. S. Harrington (a1)

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