PSR J1719−1438: Difference between revisions

PSR J1719-1438
Observation data; Epoch MJD 55411.0 Equinox J2000
Constellation	Serpens
Right ascension	17:19:10.0730(1)
Declination	−14:38:00.96(2)
Characteristics
Spectral type	millisecond pulsar
Apparent magnitude (R)	>25.4
Apparent magnitude (g)	>24.1
Apparent magnitude (I)	>22.5
Astrometry
Distance	~1,200 pc
Orbit
Primary	PSR J1719-1438
Companion	PSR J1719-1438b
Period (P)	2 hours 10 minutes 37.0237 ±0.0002 seconds
Semi-major axis (a)	0.001819(1) light seconds
Eccentricity (e)	<0.06
Periastron epoch (T)	MJD 55411.0
Details
Mass	1.4 M☉
Radius	19 km
Surface gravity (log g)	13.69 cgs
Rotation	~5.8 ms
Other designations
	PSR J1719-14
Database references
SIMBAD	data

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PSR J1719-1438 is a millisecond pulsar with a spin period of 5.8 ms located about 4,000 ly from Earth in the direction of Serpens Cauda,^[1]^[4] one minute from the border with Ophiuchus. Millisecond pulsars are generally thought to begin as normal pulsars and then spin up by accreting matter from a binary companion.

The location of PSR J1719-1438 (circled in red)

Diamond planet

The PSR J1719-1438 planetary system
Companion (in order from star)	Mass	Semimajor axis (AU)	Orbital period (hours)	Eccentricity	Inclination	Radius
b	~1.02 $M$ _J	0.004	2.176951032	<0.06	—	≤0.4 $R$ _J

PSR J1719-1438 was discovered in 2011 by the High Time Resolution Survey, a radio astronomy search for astronomical objects that rapidly vary in radio brightness, such as pulsars.^[1] Timing measurements using the Parkes Telescope and Lovell Telescope showed that it has a low-mass companion: PSR J1719-1438 b.^[1] The companion has a mass similar to that of Jupiter, but 40% of the diameter. It orbits the pulsar with a period of 2 hours 10 minutes and 37 seconds, at a distance of around 600,000 km (0.89 solar radii).^[1] The companion is likely the remnant of a star whose outer layers were siphoned off by the more massive pulsar. Calculations show the companion has a minimum density of 23 grams per cubic centimeter and is probably an ultra-low-mass carbon–oxygen white dwarf.^[1]

Because the companion to PSR J1719-1438 is planet-sized, made primarily of carbon (with an unknown amount of oxygen), and very dense, it may be similar to a large diamond. In the science press, the object has been called the "Diamond Planet".^[4]^[5]^[6]

A lump of QCD matter

It has been suggested in 2012 that PSR J1719-1438 b may not be the remnant of a white dwarf, but a lump of quark matter with a size of just 1 kilometer and the mass of Jupiter,^[7] that would have been born in the collision and merger of two previous quark stars, part of the ejected matter ending orbiting the merger remnant we see as the pulsar PSR J1719-1438.^[8]

References

^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m ⁿ Bailes, M.; Bates, S. D.; Bhalerao, V.; Bhat, N. D. R.; Burgay, M.; Burke-Spolaor, S.; d'Amico, N.; Johnston, S.; et al. (2011). "Transformation of a Star into a Planet in a Millisecond Pulsar Binary". Science. 333 (6050): 1717–20. arXiv:1108.5201. Bibcode:2011Sci...333.1717B. doi:10.1126/science.1208890. PMID 21868629. S2CID 206535504.
^ ^a ^b Tillman, Nola Taylor (25 August 2011). "Surprise! Alien Planet Made of Diamond Discovered". Space.com. Retrieved 25 August 2011.
^ van Haaften, L. M.; Nelemans, G.; Voss, R.; Jonker, P. G. "Formation of the planet around the millisecond pulsar J1719–1438" (PDF).
^ ^a ^b "Star Transforms into A Diamond Planet". Universe Today. 25 August 2011. Retrieved 26 August 2011.
^ "Surprise! Alien Planet Made of Diamond Discovered". Space.com. 25 August 2011. Retrieved 25 August 2011.
^ "A Planet made of Diamond". Max Planck Institut for Radio Astronomy. Archived from the original on 14 September 2011. Retrieved 26 August 2011.
^ Horvath, J. E. (2012). "The nature of the companion of PSR J1719-1438: a white dwarf or an exotic object?". Research in Astronomy and Astrophysics. 12 (7): 813–816. arXiv:1205.1410. Bibcode:2012RAA....12..813H. doi:10.1088/1674-4527/12/7/009. S2CID 119260648.
^ Bauswein, A.; Janka, H. -T.; Oechslin, R.; Pagliara, G.; Sagert, I.; Schaffner-Bielich, J.; Hohle, M. M.; Neuhäuser, R. (2009). "Mass Ejection by Strange Star Mergers and Observational Implications". Physical Review Letters. 103 (1): 011101. arXiv:0812.4248. Bibcode:2009PhRvL.103a1101B. doi:10.1103/PhysRevLett.103.011101. PMID 19659133. S2CID 24542292. 011101.

[bailes-1] ^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m ⁿ Bailes, M.; Bates, S. D.; Bhalerao, V.; Bhat, N. D. R.; Burgay, M.; Burke-Spolaor, S.; d'Amico, N.; Johnston, S.; et al. (2011). "Transformation of a Star into a Planet in a Millisecond Pulsar Binary". Science. 333 (6050): 1717–20. arXiv:1108.5201. Bibcode:2011Sci...333.1717B. doi:10.1126/science.1208890. PMID 21868629. S2CID 206535504.

[Space-2] Tillman, Nola Taylor (25 August 2011). "Surprise! Alien Planet Made of Diamond Discovered". Space.com. Retrieved 25 August 2011.

[Haaften-3] van Haaften, L. M.; Nelemans, G.; Voss, R.; Jonker, P. G. "Formation of the planet around the millisecond pulsar J1719–1438" (PDF).

[UniverseToday-4] "Star Transforms into A Diamond Planet". Universe Today. 25 August 2011. Retrieved 26 August 2011.

[Space.com-5] "Surprise! Alien Planet Made of Diamond Discovered". Space.com. 25 August 2011. Retrieved 25 August 2011.

[MaxPlanck-6] "A Planet made of Diamond". Max Planck Institut for Radio Astronomy. Archived from the original on 14 September 2011. Retrieved 26 August 2011.

[horvath-7] Horvath, J. E. (2012). "The nature of the companion of PSR J1719-1438: a white dwarf or an exotic object?". Research in Astronomy and Astrophysics. 12 (7): 813–816. arXiv:1205.1410. Bibcode:2012RAA....12..813H. doi:10.1088/1674-4527/12/7/009. S2CID 119260648.

[bauswein-8] Bauswein, A.; Janka, H. -T.; Oechslin, R.; Pagliara, G.; Sagert, I.; Schaffner-Bielich, J.; Hohle, M. M.; Neuhäuser, R. (2009). "Mass Ejection by Strange Star Mergers and Observational Implications". Physical Review Letters. 103 (1): 011101. arXiv:0812.4248. Bibcode:2009PhRvL.103a1101B. doi:10.1103/PhysRevLett.103.011101. PMID 19659133. S2CID 24542292. 011101.

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@@ Line 1: / Line 1: @@
+{{Short description|Millisecond pulsar in the constellation Serpens}}
-'''PSR J1719-1438''' is a [[millisecond pulsar]] with a spin period of 5.7 ms. <ref name=science>{{cite journal
+{{Use dmy dates|date=September 2014}}
- | last=Bailes | first=M.
+{{Starbox begin
- |coauthors=''et al.''
+| name = PSR J1719-1438
- | title= Transformation of a Star into a Planet in a Millisecond Pulsar Binary
+}}
- | journal= Science
+{{Starbox observe
- | doi=10.1126/science.1208890
+| epoch = [[Julian day#Alternatives|MJD]] 55411.0<ref name=bailes/><!--Epoch of observation-->
- | url=http://www.sciencemag.org/content/early/2011/08/19/science.1208890.abstract}}</ref>
+| equinox = [[J2000]]
-Millisecond pulsars are generally thought to begin as normal pulsars and then spin-up by accreting of matter from a binary companion.
+| constell = [[Serpens]]
+| pronounce = <!--Pronunciation guide-->
+| ra = 17:19:10.0730(1)<ref name=bailes/> <!--Right Ascension-->
+| dec = −14:38:00.96(2)<ref name=bailes/> <!--Declination-->
+| appmag_v =  <!--Apparent magnitude (Johnson-Cousins V system)-->
+}}
+{{Starbox character
+| class = [[millisecond pulsar]]<ref name=bailes/> <!--Stellar class-->
+| appmag_1_passband = R<!-- Passband for first apparent magnitude (e.g., H, J, K, etc.) -->
+| appmag_1 = >25.4<ref name=bailes/><!-- Value of first apparent magnitude  -->
+| appmag_2_passband = g<!-- Passband for second apparent magnitude (e.g., H, J, K, etc.) -->
+| appmag_2 = >24.1<ref name=bailes/><!-- Value of second apparent magnitude  -->
+| appmag_3_passband = I<!-- Passband for third apparent magnitude (e.g., H, J, K, etc.) -->
+| appmag_3 = >22.5<ref name=bailes/><!-- Value of third apparent magnitude  -->
+| appmag_4_passband = <!-- Passband for fourth apparent magnitude (e.g., H, J, K, etc.) -->
+| appmag_4 = <!-- Value of fourth apparent magnitude  -->
+| appmag_5_passband = <!-- Passband for fifth apparent magnitude (e.g., H, J, K, etc.) -->
+| appmag_5 = <!-- Value of fifth apparent magnitude  -->
+| appmag_6_passband = <!-- Passband for sixth apparent magnitude (e.g., H, J, K, etc.) -->
+| appmag_6 = <!-- Value of sixth apparent magnitude  -->
+| appmag_7_passband = <!-- Passband for seventh apparent magnitude (e.g., H, J, K, etc.) -->
+| appmag_7 = <!-- Value of seventh apparent magnitude  -->
+| appmag_8_passband = <!-- Passband for eighth apparent magnitude (e.g., H, J, K, etc.) -->
+| appmag_8 = <!-- Value of eighth apparent magnitude  -->
+| r-i = <!--R-I color-->
+| v-r = <!--V-R color-->
+| b-v = <!--B-V color-->
+| u-b = <!--U-B color-->
+| j-h = <!--J-H color-->
+| j-k = <!--J-K color-->
+| variable = <!--Variability type-->
+}}
+{{Starbox astrometry
+ | radial_v = <!--Radial velocity (in km/sec)-->
+ | prop_mo_ra = <!--Proper motion (RA), μ<sub>α</sub> cos δ (in milliarcsec/yr)-->
+ | prop_mo_dec = <!--Proper motion (dec), μ<sub>δ</sub> (in milliarcsec/yr)-->
+ | parallax =  <!--Parallax (in milliarcsec)-->
+ | p_error = <!--Parallax error (in milliarcsec)-->
+ | parallax_footnote = <!--Parallax footnote-->
+ | dist_ly = <!--Distance (in light years)-->
+ | dist_pc = ~1,200<ref name=bailes/><!--Distance (in parsecs)-->
+ | absmag_v = <!--Absolute magnitude ([[UBV photometric system|Johnson-Cousins V system]])-->
+ }}
+{{Starbox orbit
+| reference =<ref name=bailes/><!--Reference-->
+| primary = PSR J1719-1438<!--Primary name -->
+| name = [[PSR J1719-1438b]]<!--Companion name-->
+| period_unitless = 2 hours 10 minutes 37.0237 ±0.0002 seconds <!--Period (no units provided by template)-->
+| axis_unitless = <math>a_P\sin i=</math>0.001819(1) [[light second]]s<!--Semimajor axis (no units provided by template)-->
+| eccentricity = <0.06 <!--Eccentricity-->
+| inclination = <!--Inclination (in degrees)-->
+| node = <!--Longitude of node (in degrees)-->
+| periastron = [[Julian day#Alternatives|MJD]] 55411.0<!--Periastron epoch-->
+| periarg = <!--Argument of periastron (in degrees), secondary -->
+| periarg_primary = <!--Argument of periastron (in degrees), primary -->
+| k1 = <!-- Velocity semi-amplitude (SB1, or primary in SB2), in km/s -->
+| k2 = <!-- Velocity semi-amplitude (secondary in SB2), in km/s -->
+}}
+{{Starbox detail
+| source              =   <!--[source url]-->
+| mass                =   1.4<ref name="Space">{{cite news |last=Tillman |first=Nola Taylor |date=August 25, 2011 |title=Surprise! Alien Planet Made of Diamond Discovered |work=[[Space.com]] |publisher= |url=https://www.space.com/12731-diamond-alien-planet-discovered-neutron-star.html |access-date=August 25, 2011}}</ref>  <!--Mass (in solar masses)-->
+| radius_km           =   19<ref name="Space" />
+| gravity             =   13.69 <!--Surface gravity (given as the base 10 logarithm expressed in cgs units)-->
+| luminosity          =   <!--Luminosity (in solar luminosities); prefer luminosity_bolometric or luminosity_visual-->
+| luminosity_bolometric = <!--Luminosity (in solar luminosities), bolometric-->
+| luminosity_visual   =   <!--Luminosity (in solar luminosities), visual (V)-->
+| temperature         =   <!--Temperature (in kelvins)-->
+| metal               =   <!--Metallicity (no units provided by template)-->
+| rotation            =   ~5.8 [[millisecond|ms]]<ref name=Haaften>{{cite web|last=van Haaften|first=L. M.|last2=Nelemans|first2=G.|last3=Voss|first3=R.|last4=Jonker|first4=P. G.|url=https://www.aanda.org/articles/aa/pdf/2012/05/aa18798-12.pdf|title=Formation of the planet around the millisecond pulsar J1719–1438}}</ref> <!--Rotation (no units provided by template)-->
+| rotational_velocity =   <!--Rotational velocity (v sin i, in km/s)-->
+| age                 =   <!--Age (in years)-->
+| age_gyr             =   <!--Age (in billions of years)-->
+}}
+{{Starbox catalog
+| names = PSR J1719-14
+}}
+{{Starbox reference
+| Simbad = PSR+J1719-1438
+}}
+{{Starbox end}}
+'''PSR J1719-1438''' is a [[millisecond pulsar]] with a spin period of 5.8 ms located about 4,000 [[light year|ly]] from Earth in the direction of [[Serpens]] Cauda,<ref name=bailes/><ref name=UniverseToday/> one minute from the border with Ophiuchus. Millisecond pulsars are generally thought to begin as normal pulsars and then spin up by accreting matter from a [[Binary star|binary]] companion.
+[[File:PSRJ1719-1438Location.png|thumb|left|The location of PSR J1719-1438 (circled in red)]]
 ==Diamond planet==
+{{main|PSR J1719−1438 b}}
-Timing measurements of PSR J1719-1438 show that it has a low-mass companion. The companion has a mass similar to that of [[Jupiter]] and a diameter around 40 percent that of Jupiter. It orbits the pulsar with a period of 2.17 hours at a distance of around 600,000 km (0.89 [[Solar_radius|solar radii]]). <ref name=science/> The companion is likely the remnants of the star that the pulsar siphoned off matter from to spin up. Calculations show the companion has a minimum density of 23 [[grams]] per [[cubic centimeter]] and is probably a ultra-low mass carbon-oxygen [[white dwarf]]. <ref name=science/>
+{{Orbitbox planet begin|name=PSR J1719-1438|period_unit=hour}}{{Orbitbox planet|exoplanet=[[PSR J1719-1438 b|b]]|mass=~1.02|mass_earth=|semimajor=0.004|period=2.176951032|eccentricity=<0.06|radius=≤0.4}}{{Orbitbox end}}
+PSR J1719-1438 was discovered in 2011 by the High Time Resolution Survey, a [[radio astronomy]] search for astronomical objects that rapidly vary in radio brightness, such as pulsars.<ref name=bailes/> Timing measurements using the [[Parkes Telescope]] and [[Lovell Telescope]] showed that it has a low-mass companion: [[PSR J1719-1438 b]].<ref name=bailes/> The companion has a mass similar to that of [[Jupiter]], but 40% of the diameter. It orbits the pulsar with a period of 2 hours 10 minutes and 37 seconds, at a distance of around 600,000&nbsp;km (0.89 [[Solar radius|solar radii]]).<ref name=bailes/> The companion is likely the remnant of a star whose outer layers were siphoned off by the more massive pulsar. Calculations show the companion has a minimum density of 23 grams per cubic centimeter and is probably an ultra-low-mass carbon–oxygen [[white dwarf]].<ref name=bailes/>
-Because the companion to PSR J1719-1438 is planet sized, made primarily of carbon (with an unknown amount of oxygen), and is very dense, it may be similar to a very large diamond. In the science press, the object has been called the "Diamond Planet".
-<ref name=UniverseToday>{{cite web|title=Star Transforms Into A Diamond Planet|url=http://www.universetoday.com/88449/star-transforms-into-a-diamond-planet|work=Universe Today|accessdate=8/26/2011}}</ref>
+Because the companion to PSR J1719-1438 is planet-sized, made primarily of carbon (with an unknown amount of oxygen), and very dense, it may be similar to a large diamond. In the science press, the object has been called the [[Carbon planet|"Diamond Planet"]].<ref name=UniverseToday/><ref name=Space.com/><ref name=MaxPlanck/>
-<ref name=Space.com>{{cite web|title=Surprise! Alien Planet Made of Diamond Discovered|url=http://www.space.com/12731-diamond-alien-planet-discovered-neutron-star.html|work=Space.com|accessdate=8/25/2011}}</ref>
-<ref name= MaxPlanck>{{cite web|title=A Planet made of Diamond|url=http://www.mpifr-bonn.mpg.de/public/pr/pr-pulsar-august2011-en.html|work=Max Planck Institut for Radio Astronomy|accessdate=8/26/2011}}</ref>
+===A lump of QCD matter===
+It has been suggested in 2012 that PSR J1719-1438 b may not be the remnant of a white dwarf, but a lump of [[QCD matter|quark matter]] with a size of just 1 kilometer and the mass of Jupiter,<ref name=horvath/> that would have been born in the collision and merger of two previous [[quark star]]s, part of the ejected matter ending orbiting the merger remnant we see as the pulsar PSR J1719-1438.<ref name=bauswein/>
+== See also ==
+* {{annotated link|Black Widow Pulsar}}
+* [[EF Eridani]], a star system with a compact star and a degraded planetary-mass former star
+* {{annotated link|PSR J1544+4937}}
 ==References==
-{{reflist}}
+{{reflist|colwidth=25em|refs=
+<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.|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|bibcode = 2011Sci...333.1717B|pmid=21868629|volume=333|issue=6050|pages=1717–20|arxiv = 1108.5201 |s2cid=206535504|display-authors=8}}
+</ref>
+<ref name=UniverseToday>{{cite web|title=Star Transforms into A Diamond Planet|url=http://www.universetoday.com/88449/star-transforms-into-a-diamond-planet|work=Universe Today|date=25 August 2011|access-date=2011-08-26}}</ref><ref name=Space.com>{{cite web|title=Surprise! Alien Planet Made of Diamond Discovered|url=http://www.space.com/12731-diamond-alien-planet-discovered-neutron-star.html|work=Space.com|date=25 August 2011|access-date=2011-08-25}}</ref>
+<ref name=MaxPlanck>{{cite web|title=A Planet made of Diamond|url=http://www.mpifr-bonn.mpg.de/public/pr/pr-pulsar-august2011-en.html|work=Max Planck Institut for Radio Astronomy|access-date=2011-08-26|url-status=dead|archive-url=https://web.archive.org/web/20110914234539/http://www.mpifr-bonn.mpg.de/public/pr/pr-pulsar-august2011-en.html|archive-date=14 September 2011|df=dmy-all}}</ref>
+<ref name=horvath>{{cite journal|doi=10.1088/1674-4527/12/7/009|title=The nature of the companion of PSR J1719-1438: a white dwarf or an exotic object?|year=2012|last1=Horvath|first1=J. E.|journal=Research in Astronomy and Astrophysics|bibcode = 2012RAA....12..813H|volume=12|number=7|pages=813–816|arxiv = 1205.1410 |s2cid=119260648}}
+</ref>
+<ref name=bauswein>{{cite journal|doi=10.1103/PhysRevLett.103.011101|title=Mass Ejection by Strange Star Mergers and Observational Implications|year=2009|last1=Bauswein|first1=A.|last2=Janka|first2=H. -T.|last3=Oechslin|first3=R.|last4=Pagliara|first4=G.|last5=Sagert|first5=I.|last6=Schaffner-Bielich|first6=J.|last7=Hohle|first7=M. M.|last8=Neuhäuser|first8=R.|journal=Physical Review Letters|bibcode = 2009PhRvL.103a1101B|volume=103|issue=1|id=011101|arxiv = 0812.4248|pmid=19659133|page=011101|s2cid=24542292}}
+</ref>
+}}
+{{Stars of Serpens}}
+{{2011 in space}}
-[[pl:PSR J1719-1438]]
+{{DEFAULTSORT:PSR J1719-1438}}
+[[Category:Astronomical objects discovered in 2011|?]]
-[[pt:PSR J1719-1438]]
+[[Category:Millisecond pulsars]]
+[[Category:Planetary systems with one confirmed planet]]
+[[Category:Serpens]]

Observation data Epoch MJD 55411.0^[1] Equinox J2000
Constellation	Serpens
Right ascension	17:19:10.0730(1)^[1]
Declination	−14:38:00.96(2)^[1]
Characteristics
Spectral type	millisecond pulsar^[1]
Apparent magnitude (R)	>25.4^[1]
Apparent magnitude (g)	>24.1^[1]
Apparent magnitude (I)	>22.5^[1]
Astrometry

Distance	~1,200^[1] pc

Orbit^[1]
Primary	PSR J1719-1438
Companion	PSR J1719-1438b
Period (P)	2 hours 10 minutes 37.0237 ±0.0002 seconds
Semi-major axis (a)	$a_{P}\sin i=$ 0.001819(1) light seconds
Eccentricity (e)	<0.06
Periastron epoch (T)	MJD 55411.0
Details

Mass	1.4^[2] `M`_☉
Radius	19^[2] km
Surface gravity (log g)	13.69 cgs
Rotation	~5.8 ms^[3]

Other designations
PSR J1719-14
Database references
SIMBAD	data

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Discoveries	UDFj-39546284 Swift J1644+57 Kronberger 61 WD 0806−661 ULAS J1120+0641 Kerberos (moon) PSR J1719−1438 Uranus trojan 2011 QF99 U1.11 SDSS J102915+172927 2 moons of Jupiter GRB 111209A
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