Hostname: page-component-6bf8c574d5-n2sc8 Total loading time: 0 Render date: 2025-03-07T06:14:33.671Z Has data issue: false hasContentIssue false
  • English
  • Français

On the Role of dK and dM Stars in Piling up the Total Mass of Star Clusters

Published online by Cambridge University Press:  25 May 2016

G. Szécsényi-Nagy
G. Szécsényi-Nagy*
Affiliation:
Department of Astronomy, L. Eötvös University, H-1083 Budapest VIII. Ludovika tér 2., Hungary

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Although many projects were aimed at identifying nearby red dwarfs, the catalogues may be complete up to a limiting distance of 5 pc only and may be reliable to 10 pc. From recent observations it is evident that their absolute visual brightness (MV) ranges from about 6 to at least 18.5 what means that an average dK0 star is at least 100,000 times brighter than red dwarfs of the latest spectral subclasses. The photon detecting efficiency of our instruments is to be increased that these can measure late dM stars from the same distance from which dK stars can be analysed now. Another solution is offered by the flare-active red dwarfs which may be 1000 times brighter during their flare ups than usually.

Type
Stellar Evolution in Star Clusters
Information
Symposium - International Astronomical Union , Volume 174: Dynamical Evolution of Stars Clusters , 1996 , pp. 359 - 360
Copyright
Copyright © Kluwer 1996 

References

Benest, D. 1983, IAU Coll. 76, eds. Philip, A. G. D. & Upgren, A. R. (Schenectady: L. Davis Press Inc.) p25 Google Scholar
Rodonó, M. 1986, NASA SP-492, eds. Johnson, H. R. & Querci, F. R., p409 Google Scholar
Szécsényi-Nagy, G. 1990a, Publ. Astron. Dep. of the Eötvös Univ. No. 9., Budapest, p308 Google Scholar
Szécsényi-Nagy, G. 1990b, IAU Sym. 137, eds. Mirzoyan, L. V., Pettersen, B. R. & Tsvetkov, M. K. (Dordrecht: KAP), p71 Google Scholar