Editing PSR J0737−3039 (section)

== Physical characteristics ==
The orbital period of J0737−3039 (2.4 hours) is one of the shortest known for such an object (one-third that of the [[PSR B1913+16|Taylor–Hulse binary]]), which enables the most precise tests yet. In 2005, it was announced that measurements had shown an excellent agreement between general relativity theory and observation.  In particular, the predictions for energy loss due to [[gravitational wave]]s appear to match the theory.

As a result of energy loss due to gravitational waves, the common orbit (roughly {{Convert|800,000|km|mi|abbr=off|sp=us|disp=sqbr}} in diameter) shrinks by 7 mm per day. The two components will coalesce in about 85 million years.
:{| class=wikitable
|-
! align="left" | Property
! align="left" | Pulsar A
! align="left" | Pulsar B
|-
! Spin period
| 22.699 milliseconds
| 2.773 seconds
|-
! Mass
| 1.337 solar masses
| 1.250 solar masses
|-
! Orbital period
| colspan="2" align="center" | 2.454 hours (8834.53499 seconds)
|-
|}

Due to relativistic spin precession, the pulses from Pulsar B are no longer detectable {{As of|2008|March|lc=y}} but are expected to reappear in 2035 due to precession back into view.<ref>{{Cite journal |last1=Perera |first1=B. B. P. |last2=McLaughlin |first2=M. A. |last3=Kramer |first3=M. |last4=Stairs |first4=I. H. |last5=Ferdman |first5=R. D. |last6=Freire |first6=P. C. C. |last7=Possenti |first7=A. |last8=Breton |first8=R. P. |last9=Manchester |first9=R. N. |last10=Burgay |first10=M. |last11=Lyne |first11=A. G. |display-authors=2 |year=2010 |title=The Evolution of PSR J0737−3039B and a Model for Relativistic Spin Precession |url=https://iopscience.iop.org/article/10.1088/0004-637X/721/2/1193 |journal=[[The Astrophysical Journal]] |volume=721 |issue=2 |pages=1193–1205 |arxiv=1008.1097 |bibcode=2010ApJ...721.1193P |doi=10.1088/0004-637X/721/2/1193 |last12=Camilo |first12=F. |s2cid=118854647}}</ref>