Binary mass function: Difference between revisions

Revision as of 06:08, 16 March 2020

Revision as of 17:42, 31 May 2020

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<math>\frac{M_{2}^{3}}{M_\mathrm{tot}^{2}} = \frac{\omega_\mathrm{orb}^{2} a_{1}^{3}}{G}.</math>

The peak radial velocity of object 1, <math>K</math>, depends on the orbital inclination <math>i</math> (an inclination of 0° corresponds to an orbit seen face-on, an inclination of 90° corresponds to an orbit seen edge-on). For a circular orbit ([[orbital eccentricity]] = 0) it is given by<ref name="tauris">{{cite book |last1=Tauris |first1=T.M. |last2=van den Heuvel |first2=E.P.J. |author2-link=Ed van den Heuvel |editor1-last=Lewin |editor1-first=Walter |editor1-link=Walter Lewin |editor2-last=van der Klis |editor2-first=Michiel |editor2-link=Michiel van der Klis |title=Compact stellar X-ray sources |url=https://archive.org/details/compactstellarxr00whgl |url-access=limited |publisher=Cambridge, UK: [[Cambridge University Press]] |date=2006 |pages=623–665[https://archive.org/details/compactstellarxr00whgl/page/n640 623]–665 |chapter=Chapter 16: Formation and evolution of compact stellar X-ray sources |arxiv=astro-ph/0303456 |isbn=978-0-521-82659-4 |doi=10.2277/0521826594 |lastauthoramp=y|doi-broken-date=2020-03-16 }}</ref>

<math>K = v_{1} \mathrm{sin} i = \omega_\mathrm{orb} a_{1} \mathrm{sin} i.</math>