Perhaps the most common question that a child asks when he or she sees the night sky from a dark site for the first time is: 'How many stars are there?' This happens to be a question which has exercised the intellectual skills of many astronomers over the course of most of the last century, including, for the last two decades, one of the authors of this text. Until recently, the most accurate answer was 'We are not certain, but there is a good chance that almost all of them are M dwarfs. ' Within the last three years, results from new sky-surveys - particularly the first deep surveys at near infrared wavelengths - have provided a breakthrough in this subject, solidifying our census of the lowest-mass stars and identifying large numbers of the hitherto almost mythical substellar-mass brown dwarfs. These extremely low-luminosity objects are the central subjects of this book, and the subtitle should be interpreted accordingly. The expression 'low-mass stars' carries a wide range of meanings in the astronomical literature, but is most frequently taken to refer to objects with masses comparable with that of the Sun - F and G dwarfs, and their red giant descendants. While this definition is eminently reasonable for the average extragalactic astronomer, our discussion centres on M dwarfs, with masses of no more than 60% that of the Sun, and extends to 'failed stars' - objects with insufficient mass to ignite central hydrogen fusion.M13 Mullan, D. J., Doyle, J. G., Mathioudakis, M., Redman, R. O., 1992, in The N1 O1 O2 P1 P2 R1 R2 R3 R4 R5 R6 S1 S2 S3 S4 S5 S6 T1 T2 T3 V1 V2 W1 W2 W3 7th Cambridge Workshop on Cool ... Trimble, V., 1990, MNRAS, 242, 79.
|Title||:||New Light on Dark Stars|
|Author||:||Neill I. Reid, Suzanne L. Hawley|
|Publisher||:||Springer Science & Business Media - 2013-11-27|