astro.wikisort.org - Star

The Hulse–Taylor binary is a binary star system composed of a neutron star and a pulsar (known as PSR B1913+16, PSR J1915+1606 or PSR 1913+16) which orbit around their common center of mass. It is the first binary pulsar ever discovered.

PSR B1913+16

Observation data Epoch B1950.0      Equinox B1950.0
Constellation	Aquila[1]
Right ascension	19h 13m 12.4655s
Declination	16° 01′ 08.189″
Astrometry
Distance	21,000 ly (6,400 pc)
Details[2]
Mass	1.441 M☉
Rotation	59.02999792988 ms
Other designations
PSR B1913+16,[3] PSR J1915+1606,[3] Hulse–Taylor binary pulsar,[4] Hulse–Taylor system,[5] Hulse–Taylor binary, Hulse–Taylor pulsar,[6] Hulse–Taylor PSR[3]
Database references
SIMBAD	data

The pulsar was discovered by Russell Alan Hulse and Joseph Hooton Taylor Jr., of the University of Massachusetts Amherst in 1974. Their discovery of the system and analysis of it earned them the 1993 Nobel Prize in Physics "for the discovery of a new type of pulsar, a discovery that has opened up new possibilities for the study of gravitation."[8]

Discovery

Using the Arecibo 305 m dish, Hulse and Taylor detected pulsed radio emissions and thus identified the source as a pulsar, a rapidly rotating, highly magnetized neutron star. The neutron star rotates on its axis 17 times per second; thus the pulse period is 59 milliseconds.

After timing the radio pulses for some time, Hulse and Taylor noticed that there was a systematic variation in the arrival time of the pulses. Sometimes, the pulses were received a little sooner than expected; sometimes, later than expected. These variations changed in a smooth and repetitive manner, with a period of 7.75 hours. They realized that such behavior is predicted if the pulsar were in a binary orbit with another star, later confirmed to be another neutron star.[9]

Star system

The pulsar and its neutron star companion both follow elliptical orbits around their common center of mass. The period of the orbital motion is 7.75 hours, and the two neutron stars are believed to be nearly equal in mass, about 1.4 solar masses. Radio emissions have been detected from only one of the two neutron stars.

The minimum separation at periastron is about 1.1 solar radii; the maximum separation at apastron is 4.8 solar radii. The orbit is inclined at about 45 degrees with respect to the plane of the sky. The orientation of periastron changes by about 4.2 degrees per year in direction of the orbital motion (relativistic precession of periastron). In January 1975, it was oriented so that periastron occurred perpendicular to the line of sight from Earth.[2][10]

Use as a test of general relativity

The orbit has decayed since the binary system was initially discovered, in precise agreement with the loss of energy due to gravitational waves described by Albert Einstein's general theory of relativity.[2][10][11][12] The ratio of observed to predicted rate of orbital decay is calculated to be 0.997 ± 0.002.[12] The total power of the gravitational waves emitted by this system presently is calculated to be 7.35 × 10²⁴ watts. For comparison, this is 1.9% of the power radiated in light by the Sun. The Solar System radiates only about 5,000 watts in gravitational waves, due to the much larger distances and orbit times, particularly between the Sun and Jupiter and the relatively small mass of the planets.

With this comparatively large energy loss due to gravitational radiation, the rate of decrease of orbital period is 76.5 microseconds per year, the rate of decrease of semimajor axis is 3.5 meters per year, and the calculated lifetime to final inspiral is 300 million years.[2][12]

In 2004, Taylor and Joel M. Weisberg published a new analysis of the experimental data to date, concluding that the 0.2% disparity between the data and the predicted results is due to poorly known galactic constants, including the Sun's distance from the galactic center, the pulsar's proper motion and its distance from Earth. While there are efforts underway for better measurement of the first two quantities, they saw "little prospect for a significant improvement in knowledge of the pulsar distance," so tighter bounds will be difficult to attain. Taylor and Weisberg also mapped the pulsar's two-dimensional beam structure using the fact that the system's precession leads to varying pulse shapes. They found that the beam shape is latitudinally elongated, and pinched longitudinally near the centre, leading to an overall shape like a figure eight.[7]

In 2016, Weisberg and Huang published further results, still with a 0.16% disparity, finding that the ratio of the observed value compared to the predicted value was 0.9983 ± 0.0016.[13] They name the main driver of this improvement, from 1.8σ to 1σ discrepancy, as being improved galactic constants published in 2014.

Characteristics

• Mass of companion: 1.387 M_☉
• Total mass of the system: 2.828378(7) M_☉
• Orbital period: 7.751938773864 hr
• Eccentricity: 0.6171334
• Semi-major axis: 1,950,100 km
• Periastron separation: 746,600 km
• Apastron separation: 3,153,600 km
• Orbital velocity of stars at periastron (relative to center of mass): 450 km/s
• Orbital velocity of stars at apastron (relative to center of mass): 110 km/s

See also

• Binary pulsar
• PSR J0737−3039
• Square Kilometre Array
• Tests of general relativity
• Quadrupole formula

References

На других языках

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[de] PSR J1915+1606

PSR J1915+1606 (nach seinen Entdeckern auch Hulse-Taylor-Pulsar oder Hulse-Taylor-Doppelpulsar sowie nach älterer Nomenklatur auch PSR B1913+16) ist ein Pulsar im Sternbild Adler. Er befindet sich in einer Entfernung von 21.000 Lichtjahren. Seine Rotationsperiode beträgt mit 59,03 ms knapp 17 Umdrehungen pro Sekunde.

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- [en] Hulse–Taylor binary

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[es] PSR B1913+16

PSR B1913+16 (también conocido como J1915+1606) es un púlsar en un sistema estelar binario, en órbita con otra estrella alrededor de un centro de masa. Fue descubierto en 1974 por Russell Alan Hulse y Joseph Hooton Taylor, Jr., de la Universidad de Princeton, un descubrimiento por el que recibieron el premio Nobel de Física de 1993.

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[ru] PSR B1913+16

PSR B1913+16 (также обозначается как J1915+1606) — пульсар, представляющий собой двойную звёздную систему, состоящую из примерно одинаковых по массе звёзд, около 1,4 M⊙. Обнаружен Расселом Халсом и Джозефом Тейлором в 1974 году при проведении наблюдений на радиотелескопе обсерватории Аресибо; они были удостоены Нобелевской премии по физике в 1993 году с формулировкой «за открытие нового типа пульсаров, давшее новые возможности в изучении гравитации». Вращение звёзд происходит по вытянутым эллиптическим орбитам (эксцентриситет около 0,617), вокруг общего центра масс (период обращения 7,75 часа, минимальное сближение в системе в периастре 1,1 R⊙, максимальное удаление в апоастре 4,8 R⊙. Одна из звёзд системы — нейтронная, её период вращения около 17 оборотов в секунду (исходя из измеренного периода импульса излучения 59,03 мс). При этом средняя скорость движения по орбите около 200 км/с.

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