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<span id="openzim-page-title" class="mw-page-title-main"><span class="mw-page-title-main">X-ray binary</span></span>

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<p><b>X-ray binaries</b> are a class of <a href="Binary_star" title="Binary star">binary stars</a> that are luminous in <a href="X-ray" title="X-ray">X-rays</a>.

The X-rays are produced by matter falling from one component, called the <i>donor</i> (usually a relatively common <a href="Main_sequence" title="Main sequence">main sequence</a> <a href="Star" title="Star">star</a>), to the other component, called the <i>accretor</i>, which can be a <a href="White_dwarf" title="White dwarf">white dwarf</a>, <a href="Neutron_star" title="Neutron star">neutron star</a> or <a href="Black_hole" title="Black hole">black hole</a>.

The infalling matter releases <a href="Gravitational_energy" title="Gravitational energy">gravitational potential energy</a>, up to 30 percent of its rest mass, as X-rays. (Hydrogen <a href="Nuclear_fusion" title="Nuclear fusion">fusion</a> releases only about 0.7 percent of rest mass.) The lifetime and the mass-transfer rate in an X-ray binary depends on the evolutionary status of the donor star, the mass ratio between the stellar components, and their orbital separation.<sup id="cite_ref-Tauris_1-0" class="reference"><a href="#cite_note-Tauris-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup>

</p><p>An estimated 10<sup>41</sup> <a href="Positron" title="Positron">positrons</a> escape per second from a typical <a class="mw-selflink-fragment" href="#Low-mass_X-ray_binary">low-mass X-ray binary</a>.<sup id="cite_ref-2" class="reference"><a href="#cite_note-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-3" class="reference"><a href="#cite_note-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup>

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<div class="mw-heading mw-heading2"><h2 id="Classification">Classification</h2></div>

<p>X-ray binaries are further subdivided into several (sometimes overlapping) subclasses, that perhaps reflect the underlying physics better. Note that the classification by mass (high, intermediate, low) refers to the optically visible donor, not to the compact X-ray emitting accretor.

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<ul><li><a href="#Low-mass_X-ray_binary">Low-mass X-ray binaries</a> (LMXBs)

<ul><li><a href="Soft_X-ray_transient" title="Soft X-ray transient">Soft X-ray transients</a> (SXTs)</li>

<li><a href="Symbiotic_variable_star" class="mw-redirect" title="Symbiotic variable star">Symbiotic X-ray binaries</a></li>

<li><a href="Super_soft_X-ray_source" class="mw-redirect" title="Super soft X-ray source">Super soft X-ray sources</a> or Super soft sources<sup id="cite_ref-5" class="reference"><a href="#cite_note-5"><span class="cite-bracket">[</span>5<span class="cite-bracket">]</span></a></sup> (SSXs), (SSXB)</li>

<li>Accreting millisecond X-ray pulsars (AMXPs)<sup id="cite_ref-6" class="reference"><a href="#cite_note-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-7" class="reference"><a href="#cite_note-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup></li></ul></li>

<li><a href="#Intermediate-mass_X-ray_binary">Intermediate-mass X-ray binaries</a> (IMXBs)

<ul><li>Ultracompact X-ray binaries (UCXBs)<sup id="cite_ref-8" class="reference"><a href="#cite_note-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup></li></ul></li>

<li><a href="#High-mass_X-ray_binary">High-mass X-ray binaries</a> (HMXBs)

<ul><li><a href="Be_X-ray_binaries" class="mw-redirect" title="Be X-ray binaries">Be/X-ray binaries</a> (BeXRBs)</li>

<li><a href="X-ray_astronomy#Analytical_X-ray_astronomy" title="X-ray astronomy">Supergiant X-ray binaries</a> (SGXBs)</li>

<li><a href="X-ray_astronomy#Exotic_X-ray_sources" title="X-ray astronomy">Supergiant Fast X-ray Transients</a> (SFXTs)<sup id="cite_ref-9" class="reference"><a href="#cite_note-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-10" class="reference"><a href="#cite_note-10"><span class="cite-bracket">[</span>10<span class="cite-bracket">]</span></a></sup></li></ul></li>

<li>Others

<ul><li><a href="X-ray_burster" title="X-ray burster">X-ray bursters</a></li>

<li><a href="X-ray_pulsar" title="X-ray pulsar">X-ray pulsars</a></li>

<li><a href="#Microquasar">Microquasars</a> (radio-jet X-ray binaries that can house either a neutron star or a black hole)</li></ul></li></ul>

<div class="mw-heading mw-heading2"><h2 id="Low-mass_X-ray_binary">Low-mass X-ray binary</h2></div>

<p>A <b>low-mass X-ray binary</b> (<b>LMXB</b>) is a <a href="Binary_star" title="Binary star">binary star</a> system where one of the components is either a <a href="Black_hole" title="Black hole">black hole</a> or <a href="Neutron_star" title="Neutron star">neutron star</a>.<sup id="cite_ref-Tauris_1-1" class="reference"><a href="#cite_note-Tauris-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> The other component, a donor, usually fills its <a href="Roche_lobe" title="Roche lobe">Roche lobe</a> and therefore transfers mass to the compact star. In LMXB systems the donor is less massive than the compact object, and can be on the <a href="Main_sequence" title="Main sequence">main sequence</a>, a degenerate dwarf (<a href="White_dwarf" title="White dwarf">white dwarf</a>), or an evolved star (<a href="Red_giant" title="Red giant">red giant</a>). Approximately two hundred LMXBs have been detected in the <a href="Milky_Way" title="Milky Way">Milky Way</a>,<sup id="cite_ref-11" class="reference"><a href="#cite_note-11"><span class="cite-bracket">[</span>11<span class="cite-bracket">]</span></a></sup> and of these, thirteen LMXBs have been discovered in <a href="Globular_cluster" title="Globular cluster">globular clusters</a>. The <a href="Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a> has revealed LMXBs in many distant galaxies. <sup id="cite_ref-12" class="reference"><a href="#cite_note-12"><span class="cite-bracket">[</span>12<span class="cite-bracket">]</span></a></sup>

</p><p>A typical low-mass X-ray binary emits almost all of its <a href="Electromagnetic_radiation" title="Electromagnetic radiation">radiation</a> in <a href="X-ray" title="X-ray">X-rays</a>, and typically less than one percent in visible light, so they are among the brightest objects in the X-ray sky, but relatively faint in visible light. The <a href="Apparent_magnitude" title="Apparent magnitude">apparent magnitude</a> is typically around 15 to 20. The brightest part of the system is the <a href="Accretion_disk" title="Accretion disk">accretion disk</a> around the compact object. The orbital periods of LMXBs range from ten minutes to hundreds of days.

</p><p>The variability of LMXBs are most commonly observed as <a href="X-ray_burster" title="X-ray burster">X-ray bursters</a>, but can sometimes be seen in the form of <a href="X-ray_pulsar" title="X-ray pulsar">X-ray pulsars</a>. The <a href="X-ray_burster" title="X-ray burster">X-ray bursters</a> are created by <a href="Thermonuclear_explosion" class="mw-redirect" title="Thermonuclear explosion">thermonuclear explosions</a> created by the accretion of Hydrogen and Helium.<sup id="cite_ref-:1_13-0" class="reference"><a href="#cite_note-:1-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup>

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<div class="mw-heading mw-heading2"><h2 id="Intermediate-mass_X-ray_binary">Intermediate-mass X-ray binary</h2></div>

<p>An <b>intermediate-mass X-ray binary</b> (<b>IMXB</b>) is a binary star system where one of the components is a neutron star or a black hole. The other component is an intermediate-mass star.<sup id="cite_ref-:1_13-1" class="reference"><a href="#cite_note-:1-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-:0_14-0" class="reference"><a href="#cite_note-:0-14"><span class="cite-bracket">[</span>14<span class="cite-bracket">]</span></a></sup> An intermediate-mass X-ray binary is the origin for Low-mass X-ray binary systems.

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<div class="mw-heading mw-heading2"><h2 id="High-mass_X-ray_binary">High-mass X-ray binary</h2></div>

<p>A <b>high-mass X-ray binary</b> (<b>HMXB</b>) is a <a href="Binary_star" title="Binary star">binary star</a> system that is strong in X rays, and in which the normal stellar component is a massive <a href="Star" title="Star">star</a>: usually an O or B star, a blue <a href="Supergiant" title="Supergiant">supergiant</a>, or in some cases, a red supergiant or a <a href="Wolf%E2%80%93Rayet_star" title="Wolf–Rayet star">Wolf–Rayet star</a>.

The compact, X-ray emitting, component is a <a href="Neutron_star" title="Neutron star">neutron star</a> or <a href="Black_hole" title="Black hole">black hole</a>.<sup id="cite_ref-Tauris_1-2" class="reference"><a href="#cite_note-Tauris-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup>

A fraction of the <a href="Stellar_wind" title="Stellar wind">stellar wind</a> of the massive normal star is captured by the compact object, and produces <a href="X-ray" title="X-ray">X-rays</a> as it falls onto the compact object.

</p><p>In a high-mass X-ray binary, the massive star dominates the emission of optical light, while the compact object is the dominant source of X-rays.

The massive stars are very luminous and therefore easily detected.

One of the most famous high-mass X-ray binaries is <a href="Cygnus_X-1" title="Cygnus X-1">Cygnus X-1</a>, which was the first identified black hole candidate.

Other HMXBs include <a href="Vela_X-1" title="Vela X-1">Vela X-1</a> (not to be confused with <a href="Vela_X" class="mw-redirect" title="Vela X">Vela X</a>), and <a href="4U_1700-37" class="mw-redirect" title="4U 1700-37">4U 1700-37</a>.

</p><p>The variability of HMXBs are observed in the form of <a href="X-ray_pulsar" title="X-ray pulsar">X-ray pulsars</a> and not <a href="X-ray_burster" title="X-ray burster">X-ray bursters</a>. These <a href="X-ray_pulsar" title="X-ray pulsar">X-ray pulsars</a> are due to the accretion of matter magnetically funneled into the poles of the compact companion.<sup id="cite_ref-:1_13-2" class="reference"><a href="#cite_note-:1-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup> The <a href="Stellar_wind" title="Stellar wind">stellar wind</a> and <a href="Roche_lobe" title="Roche lobe">Roche lobe</a> overflow of the massive normal star accretes in such large quantities, the transfer is very unstable and creates a short lived mass transfer.

</p><p>Once a HMXB has reached its end, if the periodicity of the binary was less than a year, it can become a single <a href="Thorne%E2%80%93%C5%BBytkow_object" title="Thorne–Żytkow object">red giant with a neutron core</a> or a single <a href="Neutron_star" title="Neutron star">neutron star</a>. With a longer periodicity, a year and beyond, the HMXB can become a double <a href="Neutron_star" title="Neutron star">neutron star</a> binary if uninterrupted by a <a href="Supernova" title="Supernova">supernova</a>.<sup id="cite_ref-:0_14-1" class="reference"><a href="#cite_note-:0-14"><span class="cite-bracket">[</span>14<span class="cite-bracket">]</span></a></sup>

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<div class="mw-heading mw-heading2"><h2 id="Be_star_binaries">Be star binaries</h2></div>

<div class="mw-heading mw-heading3"><h3 id="Be/X-ray_binaries">Be/X-ray binaries</h3></div>

<p><a href="Be/X-ray_binary" title="Be/X-ray binary">Be/X-ray binaries</a> (BeXRBs) are a class of high-mass X-ray binaries that consist of a <a href="Be_star" title="Be star">Be star</a> and a <a href="Neutron_star" title="Neutron star">neutron star</a>. The neutron star is usually in a wide highly elliptical orbit around the Be star. The Be <a href="Stellar_wind" title="Stellar wind">stellar wind</a> forms a disk confined to a plane often different from the orbital plane of the neutron star. When the neutron star passes through the Be disk, it accretes a large mass of hot gas in a short time. As the gas falls onto the neutron star, a bright flare in hard X-rays is seen.<sup id="cite_ref-15" class="reference"><a href="#cite_note-15"><span class="cite-bracket">[</span>15<span class="cite-bracket">]</span></a></sup>

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<div class="mw-heading mw-heading3"><h3 id="Be–white_dwarf_X-ray_binary_systems">Be–white dwarf X-ray binary systems</h3></div>

<p><a href="Be%E2%80%93white_dwarf_X-ray_binary_system" title="Be–white dwarf X-ray binary system">Be–white dwarf X-ray binary systems</a> (BeWDs) are a rare type of X-ray binary consisting of a <a href="White_dwarf" title="White dwarf">white dwarf</a> that accretes matter from a rapidly-rotating <a href="Be_star" title="Be star">Be star</a>. These systems form through binary evolution where mass transfer spins up the accretor to become a Be star while the donor evolves into a white dwarf.<sup id="cite_ref-ep_17-0" class="reference"><a href="#cite_note-ep-17"><span class="cite-bracket">[</span>17<span class="cite-bracket">]</span></a></sup> Only eight BeWDs are known, though theoretical models say they should be 7 times more common than Be/neutron star binaries.

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<div class="mw-heading mw-heading2"><h2 id="Microquasar">Microquasar</h2></div>

<p>A <b>microquasar</b> (or radio emitting X-ray binary) is the smaller cousin of a <a href="Quasar" title="Quasar">quasar</a>. Microquasars are named after quasars, as they have some common characteristics: strong and variable radio emission, often resolvable as a pair of radio jets, and an <a href="Accretion_disk" title="Accretion disk">accretion disk</a> surrounding a <a href="Compact_object" title="Compact object">compact object</a> which is either a <a href="Black_hole" title="Black hole">black hole</a> or a <a href="Neutron_star" title="Neutron star">neutron star</a>. In quasars, the black hole is supermassive (millions of <a href="Solar_mass" title="Solar mass">solar masses</a>); in microquasars, the mass of the compact object is only a few solar masses. In microquasars, the accreted mass comes from a normal star, and the accretion disk is very luminous in the optical and <a href="X-ray" title="X-ray">X-ray</a> regions. Microquasars are sometimes called <i>radio-jet X-ray binaries</i> to distinguish them from other X-ray binaries. A part of the radio emission comes from <a href="Relativistic_jet" class="mw-redirect" title="Relativistic jet">relativistic jets</a>, often showing apparent <a href="Superluminal_motion" title="Superluminal motion">superluminal motion</a>.<sup id="cite_ref-18" class="reference"><a href="#cite_note-18"><span class="cite-bracket">[</span>18<span class="cite-bracket">]</span></a></sup>

</p><p>Microquasars are very important for the study of <a href="Relativistic_jet" class="mw-redirect" title="Relativistic jet">relativistic jets</a>. The jets are formed close to the compact object, and timescales near the compact object are proportional to the mass of the compact object. Therefore, ordinary quasars take centuries to go through variations a microquasar experiences in one day.

</p><p>Noteworthy microquasars include <a href="SS_433" title="SS 433">SS 433</a>, in which atomic emission lines are visible from both jets; <a href="GRS_1915%2B105" title="GRS 1915+105">GRS 1915+105</a>, with an especially high jet velocity and the very bright <a href="Cygnus_X-1" title="Cygnus X-1">Cygnus X-1</a>, detected up to the High Energy <a href="Gamma_rays" class="mw-redirect" title="Gamma rays">gamma rays</a> (E > 60 MeV). Extremely high energies of particles emitting in the VHE band might be explained by several mechanisms of particle acceleration (see <a href="Fermi_acceleration" title="Fermi acceleration">Fermi acceleration</a> and <a href="Centrifugal_mechanism_of_acceleration" class="mw-redirect" title="Centrifugal mechanism of acceleration">Centrifugal mechanism of acceleration</a>).

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<li><a href="Quasar" title="Quasar">Quasar</a></li></ul>

<div class="mw-heading mw-heading2"><h2 id="References">References</h2></div>

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</ol></div>

<div class="mw-heading mw-heading2"><h2 id="Further_reading">Further reading</h2></div>

<ul><li><cite id="CITEREFPostnovYungelson2014" class="citation journal cs1">Postnov, Konstantin A.; Yungelson, Lev R. (5 May 2014). <a rel="nofollow" class="external text" href="https://link.springer.com/article/10.12942/lrr-2014-3">"The Evolution of Compact Binary Star Systems"</a>. <i>Living Reviews in Relativity</i>. <b>17</b>.</cite></li>

<li><cite id="CITEREFNegueruelaTorrejonReigRibo2008" class="citation conference cs1">Negueruela, Ignacio; Torrejon, Jose Miguel; Reig, Pablo; Ribo, Marc; Smith, David M. (2008). <i>Supergiant Fast X-ray Transients and Other Wind Accretors</i>. A Population Explosion: The Nature & Evolution of X-Ray Binaries in Diverse Environments. Vol. 1010. pp. <span class="nowrap">252–</span>256. <a href="ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/0801.3863">0801.3863</a></span>. <a href="Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2008AIPC.1010..252N">2008AIPC.1010..252N</a>. <a href="Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1063%2F1.2945052">10.1063/1.2945052</a>. <a href="S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:18941968">18941968</a>.</cite> <a href="Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1063%2F1.2945052">10.1063/1.2945052</a> <a href="Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2008AIPC.1010..252N">2008AIPC.1010..252N</a></li></ul>

<div class="mw-heading mw-heading2"><h2 id="External_links">External links</h2></div>

<ul><li>Audio Cain/Gay (2009) <a rel="nofollow" class="external text" href="http://www.astronomycast.com/astronomy/ep-135-x-ray-astronomy/">Astronomy Cast episode 135: X-ray Astronomy</a></li>

<li><a rel="nofollow" class="external text" href="https://students.iiserkol.ac.in/~adc15rs019/ulx_pulsar_catalogue.html">Ultraluminous X-ray Pulsar (ULXP) Catalogue</a></li></ul>

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</style><div id="Neutron_star343" style="font-size:114%;margin:0 4em"><a href="Neutron_star" title="Neutron star">Neutron star</a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%">Types</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><a href="Radio-quiet_neutron_star" title="Radio-quiet neutron star">Radio-quiet</a></li>

<li><a href="Pulsar" title="Pulsar">Pulsar</a></li></ul>

</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Single pulsars</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><a href="Magnetar" title="Magnetar">Magnetar</a>

<ul><li><a href="Soft_gamma_repeater" title="Soft gamma repeater">Soft gamma repeater</a></li>

<li><a href="Anomalous_X-ray_pulsar" title="Anomalous X-ray pulsar">Anomalous X-ray</a></li>

<li>Ultra-long period</li></ul></li>

<li><a href="Rotating_radio_transient" title="Rotating radio transient">Rotating radio transient</a></li></ul>

</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Binary pulsars</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><a href="Binary_pulsar" title="Binary pulsar">Binary</a></li>

<li><a href="X-ray_pulsar" title="X-ray pulsar">X-ray pulsar</a>

<ul>

<li><a href="X-ray_burster" title="X-ray burster">X-ray burster</a></li>

<li><a href="Millisecond_pulsar" title="Millisecond pulsar">Millisecond</a></li>

<li><a href="Hulse%E2%80%93Taylor_pulsar" title="Hulse–Taylor pulsar">Hulse–Taylor pulsar</a></li></ul>

</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Properties</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><a href="Blitzar" title="Blitzar">Blitzar</a>

<ul><li><a href="Fast_radio_burst" title="Fast radio burst">Fast radio burst</a></li></ul></li>

<li><a href="Bondi_accretion" title="Bondi accretion">Bondi accretion</a></li>

<li><a href="Chandrasekhar_limit" title="Chandrasekhar limit">Chandrasekhar limit</a></li>

<li><a href="Gamma-ray_burst" title="Gamma-ray burst">Gamma-ray burst</a></li>

<li><a href="Glitch_(astronomy)" title="Glitch (astronomy)">Glitch</a></li>

<li><a href="Neutron_matter" class="mw-redirect" title="Neutron matter">Neutron matter</a></li>

<li><a href="Neutron-star_oscillation" title="Neutron-star oscillation">Neutron-star oscillation</a></li>

<li><a href="Optical_pulsar" title="Optical pulsar">Optical</a></li>

<li><a href="Pulsar_kick" title="Pulsar kick">Pulsar kick</a></li>

<li><a href="Quasi-periodic_oscillation" class="mw-redirect" title="Quasi-periodic oscillation">Quasi-periodic oscillation</a></li>

<li><a href="Relativistic_star" title="Relativistic star">Relativistic</a></li>

<li><a href="Rp-process" title="Rp-process">Rp-process</a></li>

<li><a href="Starquake_(astrophysics)" class="mw-redirect" title="Starquake (astrophysics)">Starquake</a></li>

<li><a href="Pulsar#Precise_clocks" title="Pulsar">Timing noise</a></li>

<li><a href="Tolman%E2%80%93Oppenheimer%E2%80%93Volkoff_limit" title="Tolman–Oppenheimer–Volkoff limit">Tolman–Oppenheimer–Volkoff limit</a></li>

<li><a href="Urca_process" title="Urca process">Urca process</a></li></ul>

</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Related</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><a href="Gamma-ray_burst_progenitors" title="Gamma-ray burst progenitors">Gamma-ray burst progenitors</a></li>

<li><a href="Asteroseismology" title="Asteroseismology">Asteroseismology</a></li>

<li><a href="Compact_star" class="mw-redirect" title="Compact star">Compact star</a>

<ul><li><a href="Quark_star" title="Quark star">Quark star</a></li>

<li><a href="Exotic_star" title="Exotic star">Exotic star</a></li></ul></li>

<li><a href="Supernova" title="Supernova">Supernova</a>

<ul><li><a href="Supernova_remnant" title="Supernova remnant">Supernova remnant</a></li>

<li>Related links</li></ul></li>

<li><a href="Hypernova" title="Hypernova">Hypernova</a></li>

<li><a href="Kilonova" title="Kilonova">Kilonova</a></li>

<li><a href="Microquasar" title="Microquasar">Microquasar</a></li>

<li><a href="Neutron_star_merger" title="Neutron star merger">Neutron star merger</a></li>

<li><a href="Quark-nova" title="Quark-nova">Quark-nova</a></li>

<li><a href="White_dwarf" title="White dwarf">White dwarf</a>

<ul><li>Related links</li></ul></li>

<li><a href="Stellar_black_hole" title="Stellar black hole">Stellar black hole</a>

<ul><li>Related links</li></ul></li>

<li><a href="Radio_star" title="Radio star">Radio star</a></li>

<li><a href="Pulsar_planet" title="Pulsar planet">Pulsar planet</a></li>

<li><a href="Pulsar_wind_nebula" title="Pulsar wind nebula">Pulsar wind nebula</a></li>

<li><a href="Thorne%E2%80%93%C5%BBytkow_object" title="Thorne–Żytkow object">Thorne–Żytkow object</a></li>

<li><a href="QCD_matter" title="QCD matter">QCD matter</a></li></ul>

</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Discovery</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em">

<li><a href="Centaurus_X-3" title="Centaurus X-3">Centaurus X-3</a></li>

<li><a href="Timeline_of_white_dwarfs%2C_neutron_stars%2C_and_supernovae" title="Timeline of white dwarfs, neutron stars, and supernovae">Timeline of white dwarfs, neutron stars, and supernovae</a></li></ul>

</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Satellite<br>investigation</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><a href="Rossi_X-ray_Timing_Explorer" title="Rossi X-ray Timing Explorer">Rossi X-ray Timing Explorer</a></li>

<li><a href="Fermi_Gamma-ray_Space_Telescope" title="Fermi Gamma-ray Space Telescope">Fermi Gamma-ray Space Telescope</a></li>

<li><a href="Compton_Gamma_Ray_Observatory" title="Compton Gamma Ray Observatory">Compton Gamma Ray Observatory</a></li>

<li><a href="Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a></li></ul>

</div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Other</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em">

<ul><li><a href="X-ray_pulsar-based_navigation" class="mw-redirect" title="X-ray pulsar-based navigation">X-ray pulsar-based navigation</a></li>

<li><a href="The_Magnificent_Seven_(neutron_stars)" title="The Magnificent Seven (neutron stars)">The Magnificent Seven</a></li>

<li><a href="List_of_neutron_stars" title="List of neutron stars">List of neutron stars</a>

<ul><li><a href="List_of_most_massive_neutron_stars" title="List of most massive neutron stars">Most massive neutron stars</a></li></ul></li>

<li><a href="Neutron_stars_in_fiction" title="Neutron stars in fiction">Neutron stars in fiction</a></li></ul>

</div></td></tr><tr><td class="navbox-abovebelow" colspan="2"><div>

<ul><li><span class="noviewer" typeof="mw:File"><span title="Category"></span></span> Category</li>

<li><span class="noviewer" typeof="mw:File"><span title="Commons page"></span></span> <a href="https://commons.wikimedia.org/wiki/Category:Neutron_stars" class="extiw external" title="commons:Category:Neutron stars">Commons</a></li></ul>

</div></td></tr></tbody></table></div>

<div class="navbox-styles"></div><div role="navigation" class="navbox authority-control" aria-labelledby="Authority_control_databases_frameless&#124;text-top&#124;10px&#124;alt=Edit_this_at_Wikidata&#124;link=https&#58;//www.wikidata.org/wiki/Q5961#identifiers&#124;class=noprint&#124;Edit_this_at_Wikidata642" style="padding:3px"><table class="nowraplinks hlist mw-collapsible autocollapse navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="navbox-title" colspan="2"><div id="Authority_control_databases_frameless&#124;text-top&#124;10px&#124;alt=Edit_this_at_Wikidata&#124;link=https&#58;//www.wikidata.org/wiki/Q5961#identifiers&#124;class=noprint&#124;Edit_this_at_Wikidata642" style="font-size:114%;margin:0 4em">Authority control databases </div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%">National</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"><ul><li><span class="uid"><a rel="nofollow" class="external text" href="https://id.loc.gov/authorities/sh94002242">United States</a></span></li><li><span class="uid"><a rel="nofollow" class="external text" href="https://www.nli.org.il/en/authorities/987007532463205171">Israel</a></span></li></ul></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Other</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"><ul><li><span class="uid"><a rel="nofollow" class="external text" href="https://lux.collections.yale.edu/view/concept/d9ae0e4b-9d34-4c86-8367-0b96847319ff">Yale LUX</a></span></li></ul></div></td></tr></tbody></table></div></div><div><div class="zim-footer">

This article is issued from <a class="external text" title="Last edited on 2025-07-16" href="https://en.wikipedia.org/wiki/?title=X-ray_binary&oldid=1300867951">Wikipedia</a>. The text is available under <a class="external text" href="https://creativecommons.org/licenses/by-sa/4.0/deed.en">Creative Commons Attribution-Share Alike 4.0</a> unless otherwise noted. Additional terms may apply for the media files.

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