PSR B1257+12

PSR B1257+12, alternatively designated PSR J1300+1240,^[5] is a millisecond pulsar, 2,300 light-years (710 parsecs) from the Sun, in the constellation Virgo, rotating at about 161 times per second (faster than the blade of a blender).^[2] It is also named Lich, after a powerful, fictional undead creature.^[6][4]

РSR В1257+12
Lich

Observation data Epoch J2000.0      Equinox J2000.0
Constellation	Virgo[1]
Right ascension	13h 00m 03.1075s[2]
Declination	+12° 40′ 55.155″[2]
Characteristics
Evolutionary stage	Pulsar
Astrometry
Proper motion (μ)	RA: 46.44±0.08[2] mas/yr Dec.: −84.87±0.32[2] mas/yr
Parallax (π)	1.41±0.08 mas[2]
Distance	2,300 ± 100 ly (710 ± 40 pc)
Details
Rotation	6.2185 ms[3]
Age	3±3[3] Gyr
Other designations
Lich,[4] PSR 1257+12, PSR J1300+1240, PSR 1300+1240
Database references
SIMBAD	data
Exoplanet Archive	data

The pulsar has a planetary system with three known pulsar planets, named "Draugr" (PSR B1257+12 b or PSR B1257+12 A), "Poltergeist" (PSR B1257+12 c, or PSR B1257+12 B), and "Phobetor" (PSR B1257+12 d, or PSR B1257+12 C). They were both the first extrasolar planets to be discovered and the first pulsar planets to be discovered—B and C in 1992 and A in 1994. A is the lowest-mass planet yet discovered by any observational technique, having somewhat less than twice the mass of Earth's moon.

Nomenclature

The convention that arose for designating pulsars was that of using the letters PSR (Pulsating Source of Radio) followed by the pulsar's right ascension and degrees of declination. The modern convention prefixes the older numbers with a 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. Pulsars that were discovered before 1993 tend to retain their B names rather than use their J names, but all pulsars have a J name that provides more precise coordinates of its location in the sky.^[7]

On their discovery, the planets were designated PSR 1257+12 A, B, and C, ordered by increasing distance. They were discovered before the convention that extrasolar planets receive designations consisting of the star's name followed by lower-case Roman letters starting from "b", in order of discovery, was established.^[8] However, they are listed under the latter convention on astronomical databases such as SIMBAD and the Extrasolar Planets Encyclopaedia, with A becoming b, B becoming c, and C becoming d.

In July 2014, the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars.^[9] The process involved public nomination and voting for the new names.^[10] In December 2015, the IAU announced the winning names, submitted by the Planetarium Südtirol Alto Adige in Karneid, Italy, were Lich for the pulsar and Draugr, Poltergeist, and Phobetor for planets A, B, and C, respectively:^[6][11]

• A lich is an undead creature known for controlling other undead creatures with magic.
• Draugr refers to undead creatures in Norse mythology.
• Poltergeist is a name for supernatural beings that create physical disturbances, from the German for "noisy ghost".
• Phobetor is, in Ovid's Metamorphoses, one of the thousand sons of Somnus (Sleep) who appears in dreams in the form of beasts.^[12]

In 2016, the IAU organized a Working Group on Star Names (WGSN)^[13] to catalog and standardize proper names for stars (including stellar remnants). In its first bulletin of July 2016,^[14] the WGSN explicitly recognized the names of exoplanets and their host stars approved by the Executive Committee Working Group Public Naming of Planets and Planetary Satellites, including the names of stars adopted during the 2015 NameExoWorlds campaign. This stellar remnant is now so entered in the IAU Catalog of Star Names.^[5]

Pulsar

Discovery

PSR B1257+12 was discovered by the Polish astronomer Aleksander Wolszczan on 9 February 1990 using the Arecibo radio telescope. It is a millisecond pulsar, a kind of neutron star, with a rotation period of 6.22 milliseconds (9,650 rpm), and was found to have anomalies in the pulsation period, which led to investigations as to the cause of the irregular pulses. In 1992, Wolszczan and Dale Frail published a famous paper on the first confirmed discovery of planets outside the Solar System. Using refined methods one more planet was found orbiting this pulsar in 1994.

Characteristics

The pulsar is estimated to have a mass of 1.4 M_☉, which is typical for most neutron stars and pulsars. The radius is estimated to be around 10 kilometres or 6.2 miles (~1.5×10⁻⁵ R_☉), also common for pulsars and neutron stars. The pulsar is extremely hot, with a surface temperature of up to around 28,856 K (28,583 °C; 51,481 °F). The pulsar formed one to three billion years ago from a white dwarf merger, a pair of white dwarfs colliding and collapsing to form a rapidly spinning pulsar.^[15]

The discovery stimulated a search for planets orbiting other pulsars, but it turned out such planets are rare; only a handful of other pulsar planets have been confirmed.^[16]

Planetary system

The PSR B1257+12 planetary system^[3]

Companion (in order from star)	Mass	Semimajor axis (AU)	Orbital period (days)	Eccentricity	Inclination	Radius
A (b / Draugr)	0.020 ± 0.002 M🜨	0.19	25.262 ± 0.003	0.0	~50°	—
B (c / Poltergeist)	4.3 ± 0.2 M🜨	0.36	66.5419 ± 0.0001	0.0186 ± 0.0002	53°	—
C (d / Phobetor)	3.9 ± 0.2 M🜨	0.46	98.2114 ± 0.0002	0.0252 ± 0.0002	47°	—

Planets

Artist's impression of the planets orbiting PSR B1257+12. The one in the foreground is planet "C".

In 1992, Wolszczan and Frail discovered that the pulsar had two planets. These were the first discovery of extrasolar planets to be confirmed;^[17][18] as pulsar planets, they surprised many astronomers who expected to find planets only around main-sequence stars. Additional uncertainty surrounded the system, because of a claim of an earlier pulsar planet around PSR 1829-10 that had to be retracted due to errors in calculations. In 1994, an additional planet was discovered.^[19] Additionally, this system may have an asteroid belt or a Kuiper belt.

The planets are believed to be the result of a second round of planetary system formation as a result of two white dwarfs merging with each other into a pulsar and a resulting disk of material in orbit around the star.^[15] Other scenarios include unusual supernova remnants or a quark-nova.^[20] However, the white dwarf–white dwarf merge model seems to be the most likely cause of the formation of the planets.

Retracted claim of fourth orbital body

In 1996, a possible Saturn-like (100 Earth mass) gas giant was announced orbiting the pulsar at a distance of about 40 AU (6.0 billion km; 3.7 billion mi).^[21] The original hypothesis was retracted; a reinterpretation of the data led to a new hypothesis of a dwarf planet one-fifth the size of Pluto orbiting PSR B1257+12. It would have an average orbital distance of 2.4 AU (360 million km; 220 million mi) with an orbital period of approximately 4.6 years.^{[22][23][24][25]} The dwarf planet hypothesis was also retracted because further observations showed that the pulsation anomalies previously thought to reveal a fourth orbital body are "not periodic and can be fully explained in terms of slow changes in the pulsar's dispersion measure".^[24]

See also

• 51 Pegasi
• Gamma Cephei Ab
• List of exoplanets discovered before 2000 - Draugr, Poltergeist and Phobetor
• PSR B1620-26