Binary mass function: Difference between revisions

Revision as of 20:39, 10 January 2023

Revision as of 00:27, 15 January 2023

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:<math>\frac{M_{2}^{3}}{M_\mathrm{tot}^{2}} = \frac{K^{3}}{G \omega_\mathrm{orb} \mathrm{sin}^{3} i}.</math>

The binary mass function <math>f</math> (with [[Units of measurement|unit]] of mass) is<ref name="bailes">{{cite journal|doi=10.1126/science.1208890|title=Transformation of a Star into a Planet in a Millisecond Pulsar Binary|year=2011|last1=Bailes|first1=M.|author1-link=Matthew Bailes|last2=Bates|first2=S. D.|last3=Bhalerao|first3=V.|last4=Bhat|first4=N. D. R.|last5=Burgay|first5=M.|last6=Burke-Spolaor|first6=S.|last7=d'Amico|first7=N.|last8=Johnston|first8=S.|last9=Keith|first9=M. J.|last10=Kramer|first10=M.|last11=Kulkarni|first11=S. R.|last12=Levin|first12=L.|last13=Lyne|first13=A. G.|last14=Milia|first14=S.|last15=Possenti|first15=A.|last16=Spitler|first16=L.|last17=Stappers|first17=B.|last18=Van Straten|first18=W.|journal=[[Science (journal)|Science]]|bibcode = 2011Sci...333.1717B|pmid=21868629|volume=333|issue=6050|pages=1717–1720|arxiv = 1108.5201 |s2cid=206535504|display-authors=8}}</ref><ref name="tauris" /><ref name="podsiadlowski" /><ref name="kerkwijk">{{cite journal|doi=10.1088/0004-637X/728/2/95|title=Evidence for a Massive Neutron Star from a Radial-velocity Study of the Companion to the Black-widow Pulsar PSR B1957+20|year=2011|last1= van Kerkwijk|first1=M. H.|last2=Breton|first2=MR. P.|last3=Kulkarni|first3=S. R.|author3-link=Shrinivas Kulkarni|journal=[[The Astrophysical Journal]]|bibcode = 2011ApJ...728...95V|volume=728|issue=2|pages=95|arxiv = 1009.5427|title-link=Black-widow Pulsar|s2cid=37759376}}</ref><ref name="karttunen" /><ref name="larson" /><ref>{{cite web |url=http://astronomy.swin.edu.au/cms/astro/cosmos/b/Binary+Mass+Function |title=Binary Mass Function |publisher=COSMOS – The SAO Encyclopedia of Astronomy, [[Swinburne University of Technology]] |access-date=April 20, 2016 }}</ref>

:<math>f = \frac{M_{2}^{3}\ \mathrm{sin}^{3}i }{(M_{1} + M_{2})^{2}} = \frac{P_\mathrm{orb}\ K^{3}}{2 \pi G}.</math>