PSR B1828−11

{{short description|Pulsar in the constellation Scutum}}

{{Starbox short

| name = PSR B1828-11

| epoch = J2000.0

| constell = Scutum

| ra = {{RA|18|30|47.75}}

| dec = {{DEC|-10|59|10.8}}

| appmag_v =

| absmag_v =

| dist_ly = 10,000

| dist_pc = 3,200{{cite journal|title=Pulsar timing for the Fermi gamma-ray space telescope|author=Smith, D. A.|display-authors=4|author2=Guillemot, L.|author3=Camilo, F.|author4=Cognard, I.|author5=Dumora, D.|author6=Espinoza, C.|author7=Freire, P. C. C.|author8=Gotthelf, E. V.|author9=Harding, A. K.|author10=Hobbs, G. B.|author11=Johnston, S.|author12=Kaspi, V. M.|author13=Kramer, M.|author14=Livingstone, M. A.|author15=Lyne, A. G.|author16=Manchester, R. N.|author17=Marshall, F. E.|author18=McLaughlin, M. A.|author19=Noutsos, A.|author20=Ransom, S. M.|author21=Roberts, M. S. E.|author22=Romani, R. W.|author23=Stappers, B. W.|author24=Theureau, G.|author25=Thompson, D. J.|author26=Thorsett, S. E.|author27=Wang, N.|author28=Weltevrede, P.|date=2008|journal=Astronomy and Astrophysics|volume=492|issue=3|pages=923–931|doi=10.1051/0004-6361:200810285|bibcode=2008A&A...492..923S|arxiv=0810.1637|s2cid=119200759 }}

| spectral = Pulsar

| names = PSR J1830-1059, PSR B1828-10

| Simbad = PSR+B1828-10

}}

PSR B1828-11 (also known as PSR B1828-10) is a pulsar approximately 10,000 light-years away in the constellation of Scutum. The star exhibits variations in the timing and shape of its pulses: this was at one stage interpreted as due to a possible planetary system in orbit around the pulsar, though the model required an anomalously large second period derivative of the pulse times.{{cite conference|title=Limits on pulsar planetary systems from the Jodrell Bank timing database|author=Bailes, M.|author2=Lyne, A. G.|author3=Shemar, S. L.|book-title=Planets around pulsars; Proceedings of the Conference|publisher=California Inst. of Technology, Pasadena|pages=19–30|date=1993|bibcode=1993ASPC...36...19B}} The planetary model was later discarded in favour of precession effects as the planets could not cause the observed shape variations of the pulses.{{cite journal|title=Evidence for free precession in a pulsar|author=Stairs, I. H.|author2=Lyne, A. G.|author3=Shemar, S. L.|date=2000|journal=Nature|volume=406|issue=6795|pages=484–486|bibcode=2000Natur.406..484S|doi=10.1038/35020010|pmid=10952302|s2cid=4415709 }}{{cite journal|title=Precession Interpretation of the Isolated Pulsar PSR B1828-11|author=Link, Bennett|author2=Epstein, Richard I.|journal=The Astrophysical Journal|year=2001 |volume=556|issue=1|pages=392–398|bibcode=2001ApJ...556..392L|doi=10.1086/321581|arxiv=astro-ph/0101434|s2cid=118948361 }} While the generally accepted model is that the pulsar is a neutron star undergoing free precession,{{cite journal|title=Precession of the isolated neutron star PSR B1828-11|author=Akgün, Taner|author2=Link, Bennett|author3=Wasserman, Ira|date=2006|journal=Monthly Notices of the Royal Astronomical Society|volume=365|issue=2|pages=653–672|doi=10.1111/j.1365-2966.2005.09745.x|doi-access=free |bibcode=2006MNRAS.365..653A|arxiv=astro-ph/0506606|s2cid=14390165 }} a model has been proposed that interprets the pulsar as a quark star undergoing forced precession due to an orbiting "quark planet".{{Cite journal | arxiv=astro-ph/0411133 | author=Liu | display-authors=etal | title=PSR B1828-11: a precession pulsar torqued by a quark planet?| journal=Monthly Notices of the Royal Astronomical Society: Letters | volume=381| issue=1 | pages=L1–L5| date=2007 | bibcode=2007MNRAS.381L...1L | doi=10.1111/j.1745-3933.2007.00337.x| doi-access=free | s2cid=119405995 }} The entry for the pulsar on SIMBAD lists this hypothesis as being controversial.{{cite web|url=http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=PSR+b1828-10&NbIdent=1&Radius=10&Radius.unit=arcmin&submit=submit+id|title=PSR B1828-10 -- Pulsar|website=SIMBAD|access-date=2014-07-02}}