pulsar: Definition from Answers.com

This article is about a type of neutron star. For other uses, see Pulsar (disambiguation).

Schematic view of a pulsar. The sphere in the middle represents the neutron star, the curves indicate the magnetic field lines and the protruding cones represent the emission beams.

Cycle of pulsed gamma rays from the Vela pulsar.

Pulsars are highly magnetized, rotating neutron stars that emit a beam of electromagnetic radiation. The observed periods of their pulses range from 1.4 milliseconds to 8.5 seconds.^[1] The radiation can only be observed when the beam of emission is pointing towards the Earth. This is called the lighthouse effect and gives rise to the pulsed nature that gives pulsars their name. Because neutron stars are very dense objects, the rotation period and thus the interval between observed pulses is very regular. For some pulsars, the regularity of pulsation is as precise as an atomic clock.^[2] A few pulsars are known to have planets orbiting them, as in the case of PSR B1257+12. Werner Becker of the Max Planck Institute for Extraterrestrial Physics said in 2006, "The theory of how pulsars emit their radiation is still in its infancy, even after nearly forty years of work."^[3]

1 Discovery
2 Subsequent history
3 Theory
4 Categories
5 Naming
6 Miscellaneous facts
7 Applications
8 As probes of the interstellar medium
9 Significant pulsars
10 See also
11 Notes
12 References and further reading
13 External links

Discovery

Composite Optical/X-ray image of the Crab Nebula, showing synchrotron emission in the surrounding pulsar wind nebula, powered by injection of magnetic fields and particles from the central pulsar.

The first pulsar was observed in July 1967 by Jocelyn Bell Burnell and Antony Hewish. Initially baffled as to the seemingly unnatural regularity of its emissions, they dubbed their discovery LGM-1, for "little green men" (a name for intelligent beings of extraterrestrial origin). The hypothesis that pulsars were beacons from extraterrestrial civilizations was never serious, but some discussed the far-reaching implications if it turned out to be true.^[4] Their pulsar was later dubbed CP 1919, and is now known by a number of designators including PSR 1919+21, PSR B1919+21 and PSR J1921+2153.

Although CP 1919 emits in radio wavelengths, pulsars have, subsequently, been found to emit in visible light, X-ray, and/or gamma ray wavelengths.^[5]

The word "pulsar" is a contraction of "pulsating star", and first appeared in print in 1968:

An entirely novel kind of star came to light on Aug. 6 last year and was referred to, by astronomers, as LGM (Little Green Men). Now it is thought to be a novel type between a white dwarf and a neutron [sic]. The name Pulsar is likely to be given to it. Dr. A. Hewish told me yesterday: "… I am sure that today every radio telescope is looking at the Pulsars."^[6]

The suggestion that pulsars were rotating neutron stars was put forth independently by Thomas Gold and Franco Pacini in 1968, and was soon proven beyond reasonable doubt by the discovery of a pulsar with a very short (33-millisecond) pulse period in the Crab nebula.

In 1974, Antony Hewish became the first astronomer to be awarded the Nobel Prize in physics. Considerable controversy is associated with the fact that Professor Hewish was awarded the prize while Bell, who made the initial discovery while she was his Ph.D student, was not.

Subsequent history

The Vela Pulsar and its surrounding pulsar wind nebula.

In 1974, Joseph Hooton Taylor, Jr. and Russell Hulse discovered the first time pulsar in a binary system, PSR B1913+16. This pulsar orbits another neutron star with an orbital period of just eight hours. Einstein's theory of general relativity predicts that this system should emit strong gravitational radiation, causing the orbit to continually contract as it loses orbital energy. Observations of the pulsar soon confirmed this prediction, providing the first ever evidence of the existence of gravitational waves. As of 2004, observations of this pulsar continue to agree with general relativity. In 1993, the Nobel Prize in Physics was awarded to Taylor and Hulse for the discovery of this pulsar.

In 1982, Don Backer led a group which discovered PSR B1937+21, a pulsar with a rotation period of just 1.6 milliseconds. Observations soon revealed that its magnetic field was much weaker than ordinary pulsars, while further discoveries cemented the idea that a new class of object, the "millisecond pulsars" (MSPs) had been found. MSPs are believed to be the end product of X-ray binaries. Owing to their extraordinarily rapid and stable rotation, MSPs can be used by astronomers as clocks rivaling the stability of the best atomic clocks on Earth. Factors affecting the arrival time of pulses at the Earth by more than a few hundred nanoseconds can be easily detected and used to make precise measurements. Physical parameters accessible through pulsar timing include the 3D position of the pulsar, its proper motion, the electron content of the interstellar medium along the propagation path, the orbital parameters of any binary companion, the pulsar rotation period and its evolution with time. (These are computed from the raw timing data by Tempo, a computer program specialized for this task.) After these factors have been taken into account, deviations between the observed arrival times and predictions made using these parameters can be found and attributed to one of three possibilities: intrinsic variations in the spin period of the pulsar, errors in the realization of Terrestrial Time against which arrival times were measured, or the presence of background gravitational waves. Scientists are currently attempting to resolve these possibilities by comparing the deviations seen amongst several different pulsars, forming what is known as a Pulsar Timing Array. With luck, these efforts may lead to a time scale a factor of ten or better than currently available, and the first ever direct detection of gravitational waves.

In 1992, Aleksander Wolszczan discovered the first extrasolar planets around PSR B1257+12. This discovery presented important evidence concerning the widespread existence of planets outside the solar system, although it is very unlikely that any life form could survive in the environment of intense radiation near a pulsar.

Theory

There is general agreement that what we observe as a pulse is what happens when a beam of radiation points in our direction, once for every rotation of the neutron star. The origin of the beam is related to the misalignment of the rotation axis and the axis of the magnetic field of the star. The beam is emitted from the poles of the neutron star's magnetic field, which may be offset from the rotational poles by a wide angle. The source of the power of the beam is the rotational energy of the neutron star. This rotation slows down over time as electromagnetic power is emitted.

Millisecond pulsars are thought to have been spun up to high rotational speed by matter falling in that had been pulled off from a companion star.

Of interest to the study of the state of the matter in a neutron stars are the glitches observed in the rotation velocity of the neutron star. This velocity is decreasing slowly but steadily, except by sudden variations. One model put forward to explain these glitches is that they are the result of "starquakes" that adjust the crust of the neutron star. Models where the glitch is due to a decoupling of the possibly superconducting interior of the star have also been advanced. In both cases, the star's moment of inertia changes, but its angular momentum doesn't, resulting in a change in rotation rate.

In 2003, observations of the Crab nebula's pulsar electromagnetic signal revealed "sub-pulses" within the main signal with durations of only nanoseconds. It is thought that these nanosecond pulses are emitted by regions on the pulsar's surface 60 cm in diameter or smaller, making them the smallest structures outside the solar system to be measured.

Naming

Initially pulsars were named with letters of the discovering observatory followed by their right ascension (e.g. CP 1919). As more pulsars were discovered, the letter code became unwieldy and so the convention was then superseded by the letters PSR (Pulsating Source of Radio) followed by the pulsar's right ascension and degrees of declination (e.g. PSR 0531+21) and sometimes declination to a tenth of a degree (e.g. PSR 1913+167). Pulsars that are very close together sometimes have letters appended (e.g. PSR 0021-72C and PSR 0021-72D).

The modern convention is to prefix the older numbers with a B (e.g. PSR B1919+21) with the B meaning the coordinates are for the 1950.0 epoch. All new pulsars have a J indicating 2000.0 coordinates and also have declination including minutes (e.g. PSR J1921+2153). Pulsars that were discovered before 1993 tend to retain their B names rather than use their J names (e.g. PSR J1921+2153 is more commonly known as PSR B1919+21). Recently discovered pulsars only have a J name (e.g. PSR J0437-4715). All pulsars have a J name that provides more precise coordinates of its location in the sky.^[10]

Miscellaneous facts

Lists of miscellaneous information should be avoided. Please relocate any relevant information into appropriate sections or articles. (December 2008)

The magnetic axis of pulsars determines the direction of its jets (the lighthouse spewing out the north and south poles of the magnetic axis of rotation), and their magnetic axis is not necessarily the same as their spin axis - just as Earth's magnetic north pole is not the same as its true (spin) north pole. That's why pulsars don't just "sit there" and beam at the same point in their own celestial sphere (if their outer spin axis coincided with their magnetic spin axis). If this happened, they would not pulse... there would just be detectable sources of radiation (when their jets pointed straight at us), or not, but no pulsing.
Although 8.5 seconds is the slowest observed pulsar period to date, note that as pulsars slow, their power output decreases. Conceivably there are much slower ones, below current levels of detection. On the other hand, the fastest that they can spin (e.g. 1.4 msec) seems to be dependent on the speed at which a pulsar can rotate without neutronium breaking up. In summary, young pulsars are fast and energetic; old ones are slow and weak, with the exception of millisecond pulsars, which are old but have been "recycled" to very short periods.
It is currently not known if original star mass (pre supernova) or current neutron star mass is related to pulse period.
In June 2006, the astronomer John Middleditch and his team at LANL announced the first prediction of pulsar glitches with observational data from the Rossi X-ray Timing Explorer. They used observations of the pulsar PSR J0537-6910.

Applications

The study of pulsars has resulted in many applications in physics and astronomy. Striking examples include the confirmation of the existence of gravitational radiation as predicted by general relativity and the first detection of an extrasolar planetary system.

The discovery of pulsars allowed astronomers to study an object never observed before, the neutron star. This kind of object is the only place where the behavior of matter at nuclear density can be observed (though not directly). Also, millisecond pulsars have allowed a test of general relativity in conditions of an intense gravitational field.

As probes of the interstellar medium

The radiation from pulsars passes through the interstellar medium (ISM) before reaching Earth. Free electrons in the warm (8000 K), ionized component of the ISM and H II regions affect the radiation in two primary ways. The resulting changes to the pulsar's radiation provide an important probe of the ISM itself.^[11]

Due to the dispersive nature of the interstellar plasma, lower-frequency radio waves travel through the medium slower than higher-frequency radio waves. The resulting delay in the arrival of pulses at a range of frequencies is directly measurable as the dispersion measure of the pulsar. The dispersion measure is the total column density of free electrons between the observer and the pulsar,

$\mathrm{DM} = \int_0^D n_e(s) ds,$

where $D$ is the distance from the pulsar to the observer and $n e$ is the electron density of the ISM. The dispersion measure is used to construct models of the free electron distribution in the Milky Way Galaxy.^[12]

Additionally, turbulence in the interstellar gas causes density inhomogeneities in the ISM which cause scattering of the radio waves from the pulsar. The resulting scintillation of the radio waves—the same effect as the twinkling of a star in visible light due to density variations in the Earth's atmosphere—can be used to reconstruct information about the small scale variations in the ISM.^[13] Due to the high velocity (up to several hundred km/s) of many pulsars, a single pulsar scans the ISM rapidly, which results in changing scintillation patterns over timescales of a few minutes.^[14]

Significant pulsars

Gamma-ray pulsars detected by the Fermi Gamma-ray Space Telescope.

The first radio pulsar CP 1919 (now known as PSR 1919+21), with a pulse period of 1.337 seconds and a pulse width of 0.04 second, was discovered in 1967.^[15] A drawing of this pulsar's radio waves was used as the cover of British rock band Joy Division's debut album, "Unknown Pleasures".
The first binary pulsar, PSR 1913+16, whose orbit is decaying at the exact rate predicted due to the emission of gravitational radiation by general relativity
The first millisecond pulsar, PSR B1937+21
The brightest millisecond pulsar, PSR J0437-4715
The first X-ray pulsar, Cen X-3
The first accreting millisecond X-ray pulsar, SAX J1808.4-3658
The first pulsar with planets, PSR B1257+12
The first double pulsar binary system, PSR J0737−3039
The longest period pulsar, PSR J2144-3933
The most stable pulsar in period, PSR J0437-4715
The magnetar SGR 1806-20 produced the largest burst of power in the Galaxy ever experimentally recorded on 27 December 2004^[16]

PSR B1931+24 "... appears as a normal pulsar for about a week and then 'switches off' for about one month before emitting pulses again. [..] this pulsar slows down more rapidly when the pulsar is on than when it is off. [.. the] braking mechanism must be related to the radio emission and the processes creating it and the additional slow-down can be explained by the pulsar wind leaving the pulsar's magnetosphere and carrying away rotational energy.^[17]

PSR J1748-2446ad, at 716 Hz, the pulsar with the highest rotation speed.

PSR J0108-1431, the closest known pulsar to the Earth. It lies in the direction of the constellation Cetus, at a distance of about 85 parsecs (280 light years). Nevertheless, it was not discovered until 1993 due to its extremely low luminosity. It was discovered by the Danish astronomer Thomas Tauris.^[18] in collaboration with a team of Australian and European astronomers using the Parkes 64-meter radio telescope. The pulsar is 1000 times weaker than an average radio pulsar and thus this pulsar may represent the tip of an iceberg of a population of more than half a million such dim pulsars crowding our Milky Way.^[19]^[20]

PSR J1903+0327, a ~2.15 ms pulsar discovered to be in a highly eccentric binary star system with a sun-like star.^[21]

A pulsar in the CTA 1 supernova remnant initially emitted radiation in the X-ray bands. Strangely, when it was observed at a later time X-ray radiation was not detected. Instead, the Fermi Gamma-ray Space Telescope detected the pulsar was emitting gamma ray radiation, the first of its kind.^[7]

Notes

^ Young, M.D.; Manchester, R.N.; Johnston, S. "A Radio Pulsar with an 8.5-Second Period that Challenges Emission Models." Nature, Volume 400, 26 August 1999 (pages 848-849).
^ D.N. Matsakis, J.H. Taylor and T.M. Eubanks. "A Statistic for Describing Pulsar and Clock Stabilities." Astronomy and Astrophysics, Volume 326, October 1997 (pages 924-928).
^ Press Release: Old Pulsars Still Have New Tricks to Teach Us. European Space Agency, 26 July 2006.
^ Sturrock, Peter A. The UFO Enigma: A New Review of the Physical Evidence. Warner Books, 1999 (page 154).
^ Courtland, Rachel. "Pulsar Detected by Gamma Waves Only." New Scientist, 17 October 2008.
^ Daily Telegraph, 21/3, 5 March 1968.
^ ^a ^b Atkinson, Nancy. "Fermi Telescope Makes First Big Discovery: Gamma Ray Pulsar." Universe Today, 17 October 2008.
^ NASA'S Fermi Telescope Unveils a Dozen New Pulsars http://www.nasa.gov/mission_pages/GLAST/news/dozen_pulsars.html
^ Cosmos Online - New Kind of pulsar discovered (http://www.cosmosmagazine.com/news/2260/new-kind-pulsar-discovered)
^ Lyne, Andrew G.; Graham-Smith, Francis. Pulsar Astronomy. Cambridge University Press, 1998.
^ Ferriere, K. "The Interstellar Environment of Our Galaxy." Reviews of Modern Physics, Volume 73, Issue 4, 2001 (pages 1031–1066).
^ Taylor, J. H.; Cordes, J. M. "Pulsar Distances and the Galactic Distribution of Free Electrons." Astrophysical Journal, Volume 411, 1993 (page 674).
^ Rickett, Barney J. "Radio Propagation Through the Turbulent Interstellar Plasma." Annual Review of Astronomy and Astrophysics, Volume 28, 1990 (page 561).
^ Rickett, Barney J.; Lyne, Andrew G.; Gupta, Yashwant. "Interstellar Fringes from Pulsar B0834+06." Monthly Notices of the Royal Astronomical Society, Volume 287, 1997 (page 739).
^ Hewish, A. et al. "Observation of a Rapidly Pulsating Radio Source." Nature, Volume 217, 1968 (pages 709-713).
^ "Galactic Magnetar Throws Giant Flare." Astronomy Picture of the Day, 21 February 2005.
^ "Part-Time Pulsar Yields New Insight Into Inner Workings of Cosmic Clocks." Particle Physics and Astronomy Research Council, 3 March 2006.
^ Tauris, T. M. et al. "Discovery of PSR J0108-1431: The Closest Known Neutron Star?" Astrophysical Journal, Volume 428, 1994 (page L53).
^ Crowsell, K. "Science: Dim Pulsars May Crowd Our Galaxy." New Scientist, Number 1930, 18 June 2008. (page 16).
^ "Closest Pulsar?" Sky & Telescope, October 1994 (page 14).
^ Champion, David J. et al. "An Eccentric Binary Millisecond Pulsar in the Galactic Plane." Science, 6 June 2008 Volume 320, Number 5881 (pages 1309-1312).

References and further reading

Lorimer, Duncan R. "Binary and Millisecond Pulsars at the New Millennium." Living Reviews, Relativity 4, 2001.
Lorimer, Duncan R.; Kramer, M. "Handbook of Pulsar Astronomy." Cambridge Observing Handbooks for Research Astronomers, 2004.
Stairs, Ingrid H. "Testing General Relativity with Pulsar Timing." Living Reviews, Relativity 6, 2003.
Sturrock, Peter A. The UFO Enigma: A New Review of the Physical Evidence. Warner Books, 1999 (ISBN 0-446-52565-0).

External links

Wikimedia Commons has media related to: Pulsars

"Pinning Down a Pulsar’s Age". Science News.
"Astronomical whirling dervishes hide their age well". Astronomy Now.
Animation of a Pulsar. Einstein.com, 17 January 2008.
"The Discovery of Pulsars." BBC, 23 December 2002.
"A Pulsar Discovery: First Optical Pulsar." Moments of Discovery, American Institute of Physics, 2007 (Includes audio and teachers guides).
Discovery of Pulsars: Interview with Jocelyn Bell-Burnell. Jodcast, June 2007 (Low Quality Version).
Listing for PULS CP 1919 (The First Pulsar), Simbad Database
Australia National Telescope Facility: Pulsar Catalogue
Johnston, William Robert. "List of Pulsars in Binary Systems." Johnston Archive, 22 March 2005.
Staff Writers. "Scientists Can Predict Pulsar Starquakes." Space Daily, 7 June 2006.
Staff Writers. "XMM-Newton Makes New Discoveries About Old Pulsars." Space Daily, 27 July 2006.
Than, Ker. "Hot New Idea: How Dead Stars Go Cold." Space.com, 27 July 2006.
"New Kind of Pulsar Discovered"[1]. Cosmos Online.

v • d • e Neutron star

Types	Radio-quiet · Pulsar

Single pulsars	Rotation-powered · Magnetar (Soft gamma repeater · Anomalous X-ray) · Rotating radio transient

Binary pulsars	Binary · X-ray (X-ray binary · X-ray burster · List) · Millisecond · Be/X-ray · Spin-up

Properties	Neutron-star oscillations · Neutronium · Tolman-Oppenheimer-Volkoff limit · Rp-process · Gamma-ray burst · Optical · Timing noise · Relativistic · Glitch · Pulsar kicks · Bondi accretion · Quasi-periodic oscillations · Urca process

Related	Compact star (Exotic star · Quark star · Preon star · Q star) · Supernova (Supernova remnant) · Hypernova · Quark nova · White dwarf · Stellar black hole · Radio star · Pulsar planet · Pulsar wind nebula · Thorne-Żytkow object

Discovery	LGM-1 · Centaurus X-3 · Timeline of white dwarfs, neutron stars, and supernovae

Satellite Investigation of	Rossi X-ray Timing Explorer · Fermi Gamma-ray Space Telescope · Compton Gamma Ray Observatory · Chandra X-ray Observatory

Other	X-ray pulsar based navigation · Tempo software program · Astropulse

v • d • e Star

Evolution	Formation · Pre-main sequence · Main sequence · Horizontal branch · Asymptotic giant branch · Instability strip · Red clump · Planetary nebula · Protoplanetary nebula · Luminous blue variable · Wolf-Rayet star · Supernova impostor · Supernova · Hypernova · Hertzsprung–Russell diagram

Protostars	Molecular cloud · Bok globule · Young stellar object · Herbig–Haro object · Hayashi track · Hayashi limit · Henyey track · T Tauri star · Herbig Ae/Be star

Types	Subdwarf · Dwarf (Blue · Orange · Red · Yellow) · Subgiant · Giant (Red) · Bright giant · Supergiant (Blue · Red · Yellow) · Hypergiant (Yellow) · Blue straggler · Shell · Carbon (CH) · Barium · S-type · Peculiar · Technetium · Mercury-manganese · Variable · Dark matter dark star

Remnants	White dwarf (Black dwarf) · Neutron star (Pulsar · Magnetar) · Stellar black hole

Exotic compact star	Quark star · Preon star · Q star · Fuzzball · Boson star · Gravastar · Dark energy star · Black star · Eternally collapsing object

Failed stars	Brown dwarf · Sub-brown dwarf · Planetar

Structure	Core · Convection zone · Radiation zone · Photosphere · Starspot · Chromosphere · Corona · Stellar wind · Stellar wind bubble · Asteroseismology · Eddington luminosity

Nucleosynthesis	Alpha process · Triple-alpha process · Proton-proton chain · Helium flash · CNO cycle · Carbon burning · Neon burning · Oxygen burning · Silicon burning · S-process · R-process

Properties	Classification · Designation · Dynamics · Effective temperature · Kinematics (Proper motion · Radial velocity) · Magnetic field · Magnitude (Absolute · Apparent · Photographic) · Mass · Metallicity · Microturbulence · Oscillations · Planetary system · Rotation · Star system (Binary · Contact binary · Multiple) · UBV color

Lists	Star names · Most massive · Least massive · Largest · Brightest · Most luminous · Nearest · Brown dwarfs · Timeline of stellar astronomy

Obsolete science	Newtonian dark star

v • d • e Supernova

Classes	Type Ia · Type Ib and Ic · Type II (IIP and IIL)

Related	Near-Earth supernova · Supernova impostor · Hypernova · Quark-nova · Pulsar kicks

Structure	Pair-instability supernova · Supernova nucleosynthesis · P-process · R-process · Gamma-ray burst · Carbon detonation

Progenitors	Luminous blue variable · Wolf-Rayet star · Supergiant (Blue · Red · Yellow) · Hypergiant (Yellow) · White dwarf

Remnants	Supernova remnant · Neutron star (Pulsar · Magnetar) · Stellar black hole · Compact star (Exotic star · Quark star · Preon star · Q star)

Discovery	Guest star · History of supernova observation · Timeline of white dwarfs, neutron stars, and supernovae

Lists	Notable supernovae · Supernova remnants · Massive stars

Notable	Crab (Crab Nebula) · Tycho's · Kepler's · SN 1987A in the LMC · SN 185 · SN 1006 · SN 2003fg · Vela Remnant · Remnant G1.0+0.3

Research	Supernova Cosmology Project · High-z Supernova Search Team · Texas Supernova Search · Nearby Supernova Factory · Supernova Legacy Survey · Supernova Early Warning System · Monte Agliale Supernovae and Asteroid Survey · Supernova/Acceleration Probe · Sloan Supernova Survey

In Fiction	Supernovae in fiction · Supernova weapons in science fiction

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