View source for PSR J2144−3933

{{Short description|Star in the constellation Grus}}
{{Starbox begin
| name=PSR J2144−3933}}
{{Starbox observe
| epoch=J2000
| ra={{RA|21|44|12.10}}
| dec={{DEC|−39|33|55.2}}
| appmag_v=
| constell=[[Grus (constellation)|Grus]] }}
{{Starbox character
| class=Pulsar
| b-v=
| u-b=
| variable=None }}
{{Starbox astrometry
| radial_v=
| prop_mo_ra=
| prop_mo_dec=
| parallax=
| p_error=
| absmag_v=
| dist_ly=approx. 587
| dist_pc=approx. 180
}}
{{Starbox detail
| mass=
| radius=
| luminosity=
| temperature=
| metal=
| rotation=8.51 [[second|s]]
| age= }}
{{Starbox catalog
| names=EUVE J2144-39.6 }}
{{Starbox reference
| Simbad = PSR+J2144−3933
}}
{{Starbox end}}
'''PSR J2144−3933''' is a [[pulsar]] about 180 [[parsec]]s (587 light-years) from Earth. It is the coldest known [[neutron star]] with a surface temperature less than 42000 Kelvin as measured by the [[Hubble Space Telescope]].<ref name="HSTcoldest">{{cite journal|title=Hubble Space Telescope Nondetection of PSR J2144–3933: The Coldest Known Neutron Star|first1=S.|last1=Guillot|first2=G.G.|last2=Pavlov|first3=C.|last3=Reyes|first4=A.|last4=Reisenegger|first5=L.E.|last5=Rodriguez|first6=B.|last6=Rangelov|first7=O.|last7=Kargaltsev|journal=[[The Astrophysical Journal (journal)|The Astrophysical Journal]]|issue=2|pages=175|date=5 April 2019|volume=874|doi=10.3847/1538-4357/ab0f38|arxiv=1901.07998|bibcode=2019ApJ...874..175G|s2cid=85543077 |doi-access=free }}</ref> It was previously thought to have a period of 2.84 seconds but is now known to have a period of 8.51 seconds, which is among the longest-known [[radio pulsar]].

J2144−3933 is also notable for other reasons: its [[mean pulse profile]] is very narrow in comparison to the pulse period with a half-intensity width of less than one degree of longitude.  It also has the lowest [[spindown luminosity]] of any pulsar at about 3×10<sup>21</sup> [[watt]]s.

Writing in ''[[Nature (journal)|Nature]]'', astrophysicists [[M. D. Young]] and coworkers consider this object and suggest that its existence throws current theories into doubt.  They state:

:''Moreover, under the usual model assumptions, based on the neutron-star [[equation of state|equations of state]], this slowly rotating pulsar should not be emitting a radio beam. Therefore either the model assumptions are wrong, or current theories of radio emission must be revised''<ref name="Nature400">{{cite journal|url=http://hera.ph1.uni-koeln.de/~heintzma/NS1/sub/J2144-3933.htm|title=A radio pulsar with an 8.5-second period that challenges emission models|first1=M. D.|last1=Young|first2=R. N.|last2=Manchester|first3=S.|last3=Johnston|journal=[[Nature (journal)|Nature]]|issue=6747|pages=848–849|date=26 August 1999|volume=400|doi=10.1038/23650|bibcode=1999Natur.400..848Y|s2cid=4358706|url-status=dead|archiveurl=https://archive.today/20130629090115/http://hera.ph1.uni-koeln.de/~heintzma/NS1/sub/J2144-3933.htm|archivedate=29 June 2013|url-access=subscription}}</ref>

The fact that J2144−3933 is the coldest observed neutron star has been exploited to constrain the properties of [[dark matter]].<ref>{{cite journal |last1=McKeen |first1=D. |last2=Pospelov |first2=M.|last3=Raj |first3=N. |date=Jun 3, 2021 |title=Cosmological and astrophysical probes of dark baryons |journal=Physical Review D |volume=103 |issue=11 |page=115002 |url=https://doi.org/10.1103/PhysRevD.103.115002|doi=10.1103/PhysRevD.103.115002|arxiv=2012.09865 |bibcode=2021PhRvD.103k5002M |s2cid=229332100 }}</ref><ref>{{cite journal |last1=McKeen |first1=D. |last2=Pospelov |first2=M.|last3=Raj |first3=N. |date=Aug 6, 2021 |title=Neutron Star Internal Heating Constraints on Mirror Matter|journal=Physical Review Letters |volume=127 |issue=6 |page=061805 |url=https://doi.org/10.1103/PhysRevLett.127.061805|doi=10.1103/PhysRevLett.127.061805 |pmid=34420351 |arxiv=2105.09951 |bibcode=2021PhRvL.127f1805M |s2cid=235125629 }}</ref><ref>{{cite journal |last1=Bramante |first1=J. |last2=Kavanaugh |first2=B.|last3=Raj |first3=N. |title=Scattering Searches for Dark Matter in Subhalos: Neutron Stars, Cosmic Rays, and Old Rocks|journal=Physical Review Letters |year=2022 |volume=128 |issue=23 |page=231801 |doi=10.1103/PhysRevLett.128.231801 |pmid=35749183 |arxiv=2109.04582 |bibcode=2022PhRvL.128w1801B |s2cid=237485354 }}</ref>

==References==
{{reflist}}

==External links==
* http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=PSR+J2144-3933&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id
*{{cite web|url=https://www.sciencedaily.com/releases/1999/08/990825183711.htm|title="Undead" Star Torpedoes Current Theories|date=26 August 1999|publisher=Sciencedaily.com|accessdate=June 28, 2013}}
*{{cite news|url=http://astrobites.org/2011/03/25/a-pulsar-alone/|title=A Pulsar Alone: The first deep X-ray and optical observations of the closest isolated radio pulsar|last=Kohler|first=Susanna|newspaper=[[Astrobites]] |publisher=Astrobites.org|date=25 March 2011|accessdate=June 28, 2013}}

{{Neutron star}}
{{Grus (constellation)}}

{{DEFAULTSORT:PSR J2144-3933}}
[[Category:Rotation-powered pulsars]]
[[Category:Grus (constellation)]]


{{var-star-stub}}
{{Sky|21|44|12.10|−|39|33|55.2|587}}