Magnetar

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Artist's conception of a powerful magnetar in a star cluster Artist's impression of the magnetar in the star cluster Westerlund 1.jpg
Artist's conception of a powerful magnetar in a star cluster

A magnetar is a type of neutron star with an extremely powerful magnetic field (~109 to 1011 T, ~1013 to 1015 G). [1] The magnetic-field decay powers the emission of high-energy electromagnetic radiation, particularly X-rays and gamma rays. [2]

Contents

The existence of magnetars was proposed in 1992 by Robert Duncan and Christopher Thompson. [3] Their proposal sought to explain the properties of transient sources of gamma rays, now known as soft gamma repeaters (SGRs). [4] [5] Over the following decade, the magnetar hypothesis became widely accepted, and was extended to explain anomalous X-ray pulsars (AXPs). As of July 2021, 24 magnetars have been confirmed. [6]

It has been suggested that magnetars are the source of fast radio bursts (FRB), in particular as a result of findings in 2020 by scientists using the Australian Square Kilometre Array Pathfinder (ASKAP) radio telescope. [7]

Description

Like other neutron stars, magnetars are around 20 kilometres (12 mi) in diameter, and have a mass of about 1.4 solar masses. They are formed by the collapse of a star with a mass 10–25 times that of the Sun. The density of the interior of a magnetar is such that a tablespoon of its substance would have a mass of over 100 million tons. [2] Magnetars are differentiated from other neutron stars by having even stronger magnetic fields, and by rotating more slowly in comparison. Most observed magnetars rotate once every two to ten seconds, [8] whereas typical neutron stars, observed as radio pulsars, rotate one to ten times per second. [9] A magnetar's magnetic field gives rise to very strong and characteristic bursts of X-rays and gamma rays. The active life of a magnetar is short compared to other celestial bodies. Their strong magnetic fields decay after about 10,000 years, after which activity and strong X-ray emission cease. Given the number of magnetars observable today, one estimate puts the number of inactive magnetars in the Milky Way at 30 million or more. [8]

Starquakes triggered on the surface of the magnetar disturb the magnetic field which encompasses it, often leading to extremely powerful gamma-ray flare emissions which have been recorded on Earth in 1979, 1998 and 2004. [10]

Neutron Star Types (24 June 2020) PIA23863-NeutronStars-Types-20200624.jpg
Neutron Star Types (24 June 2020)

Magnetic field

Magnetars are characterized by their extremely powerful magnetic fields of ~109 to 1011 T. [6] These magnetic fields are a hundred million times stronger than any man-made magnet, [11] and about a trillion times more powerful than the field surrounding Earth. [12] Earth has a geomagnetic field of 30–60 microteslas, and a neodymium-based, rare-earth magnet has a field of about 1.25 tesla, with a magnetic energy density of 4.0 × 105 J/m3. A magnetar's 1010 tesla field, by contrast, has an energy density of 4.0×1025 J/m3, with an E/c2 mass density more than 10,000 times that of lead. The magnetic field of a magnetar would be lethal even at a distance of 1,000 km due to the strong magnetic field distorting the electron clouds of the subject's constituent atoms, rendering the chemistry of sustaining life impossible. [13] At a distance of halfway from Earth to the moon, an average distance between the Earth and the Moon being 384,400 km (238,900 miles), a magnetar could wipe information from the magnetic stripes of all credit cards on Earth. [14] As of 2020, they are the most powerful magnetic objects detected throughout the universe. [10] [15]

As described in the February 2003 Scientific American cover story, remarkable things happen within a magnetic field of magnetar strength. "X-ray photons readily split in two or merge. The vacuum itself is polarized, becoming strongly birefringent, like a calcite crystal. Atoms are deformed into long cylinders thinner than the quantum-relativistic de Broglie wavelength of an electron." [4] In a field of about 105 teslas atomic orbitals deform into rod shapes. At 1010 teslas, a hydrogen atom becomes 200 times as narrow as its normal diameter. [4]

Origins of magnetic fields

The dominant model of the strong fields of magnetars is that it results from a magnetohydrodynamic dynamo process in the turbulent, extremely dense conducting fluid that exists before the neutron star settles into its equilibrium configuration. [16] These fields then persist due to persistent currents in a proton-superconductor phase of matter that exists at an intermediate depth within the neutron star (where neutrons predominate by mass). A similar magnetohydrodynamic dynamo process produces even more intense transient fields during coalescence of pairs of neutron stars. [17] An alternative model is that they simply result from the collapse of stars with unusually strong magnetic fields. [18]

Formation

Magnetar SGR 1900+14 (center of image) showing a surrounding ring of gas 7 light-years across in infrared light, as seen by the Spitzer Space Telescope. The magnetar itself is not visible at this wavelength but has been seen in X-ray light. Dust Ring around Magnetar1.jpg
Magnetar SGR 1900+14 (center of image) showing a surrounding ring of gas 7 light-years across in infrared light, as seen by the Spitzer Space Telescope. The magnetar itself is not visible at this wavelength but has been seen in X-ray light.

In a supernova, a star collapses to a neutron star, and its magnetic field increases dramatically in strength through conservation of magnetic flux. Halving a linear dimension increases the magnetic field strength fourfold. Duncan and Thompson calculated that when the spin, temperature and magnetic field of a newly formed neutron star falls into the right ranges, a dynamo mechanism could act, converting heat and rotational energy into magnetic energy and increasing the magnetic field, normally an already enormous 108 teslas, to more than 1011 teslas (or 1015 gauss). The result is a magnetar. [19] It is estimated that about one in ten supernova explosions results in a magnetar rather than a more standard neutron star or pulsar. [20]

1979 discovery

On March 5, 1979, a few months after the successful dropping of landers into the atmosphere of Venus, the two uncrewed Soviet spaceprobes Venera 11 and 12, then in heliocentric orbit, were hit by a blast of gamma radiation at approximately 10:51 EST. This contact raised the radiation readings on both the probes from a normal 100 counts per second to over 200,000 counts a second in only a fraction of a millisecond. [4]

Eleven seconds later, Helios 2, a NASA probe, itself in orbit around the Sun, was saturated by the blast of radiation. It soon hit Venus, where the Pioneer Venus Orbiter's detectors were overcome by the wave. Shortly thereafter the gamma rays inundated the detectors of three U.S. Department of Defense Vela satellites, the Soviet Prognoz 7 satellite, and the Einstein Observatory, all orbiting Earth. Before exiting the solar system the radiation was detected by the International Sun–Earth Explorer in halo orbit. [4]

This was the strongest wave of extra-solar gamma rays ever detected at over 100 times as intense as any previously known burst. Given the speed of light and its detection by several widely dispersed spacecraft, the source of the gamma radiation could be triangulated to within an accuracy of approximately 2 arcseconds. [21] The direction of the source corresponded with the remnants of a star that had gone supernova around 3000 BCE. [10] It was in the Large Magellanic Cloud and the source was named SGR 0525-66; the event itself was named GRB 790305b, the first-observed SGR megaflare.

Recent discoveries

Artist's impression of a gamma-ray burst and supernova powered by a magnetar Artist's impression of a gamma-ray burst and supernova powered by a magnetar.jpg
Artist's impression of a gamma-ray burst and supernova powered by a magnetar

On February 21, 2008, it was announced that NASA and researchers at McGill University had discovered a neutron star with the properties of a radio pulsar which emitted some magnetically powered bursts, like a magnetar. This suggests that magnetars are not merely a rare type of pulsar but may be a (possibly reversible) phase in the lives of some pulsars. [23] On September 24, 2008, ESO announced what it ascertained was the first optically active magnetar-candidate yet discovered, using ESO's Very Large Telescope. The newly discovered object was designated SWIFT J195509+261406. [24] On September 1, 2014, ESA released news of a magnetar close to supernova remnant Kesteven 79. Astronomers from Europe and China discovered this magnetar, named 3XMM J185246.6+003317, in 2013 by looking at images that had been taken in 2008 and 2009. [25] In 2013, a magnetar PSR J1745−2900 was discovered, which orbits the black hole in the Sagittarius A* system. This object provides a valuable tool for studying the ionized interstellar medium toward the Galactic Center. In 2018, the temporary result of the merger of two neutron stars was determined to be a hypermassive magnetar, which shortly collapsed into a black hole. [26]

In April 2020, a possible link between fast radio bursts (FRBs) and magnetars was suggested, based on observations of SGR 1935+2154, a likely magnetar located in the Milky Way galaxy. [27] [28] [29] [30] [31]

Known magnetars

On 27 December 2004, a burst of gamma rays from SGR 1806-20 passed through the Solar System (artist's conception shown). The burst was so powerful that it had effects on Earth's atmosphere, at a range of about 50,000 light-years. SGR 1806-20 108530main cloudballPrint.jpg
On 27 December 2004, a burst of gamma rays from SGR 1806−20 passed through the Solar System (artist's conception shown). The burst was so powerful that it had effects on Earth's atmosphere, at a range of about 50,000 light-years.

As of July 2021, 24 magnetars are known, with six more candidates awaiting confirmation. [6] A full listing is given in the McGill SGR/AXP Online Catalog. [6] Examples of known magnetars include:

Magnetar—SGR J1745-2900
Magnetar-SGR1745-2900-20150515.jpg
Magnetar found very close to the supermassive black hole, Sagittarius A*, at the center of the Milky Way galaxy

Bright supernovae

Unusually bright supernovae are thought to result from the death of very large stars as pair-instability supernovae (or pulsational pair-instability supernovae). However, recent research by astronomers [41] [42] has postulated that energy released from newly formed magnetars into the surrounding supernova remnants may be responsible for some of the brightest supernovae, such as SN 2005ap and SN 2008es. [43] [44] [45]

Related Research Articles

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<span class="mw-page-title-main">SGR 1806−20</span> A magnetar, a type of neutron star, with the most powerful magnetic field known

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References

Specific

  1. ↑ Kaspi, Victoria M.; Beloborodov, Andrei M. (2017). "Magnetars". Annual Review of Astronomy and Astrophysics. 55 (1): 261–301. arXiv: 1703.00068 . Bibcode:2017ARA&A..55..261K. doi:10.1146/annurev-astro-081915-023329.
  2. 1 2 Ward; Brownlee, p.286
  3. ↑ Duncan, Robert C.; Thompson, Christopher (1992). "Formation of Very Strongly Magnetized Neutron Stars: Implications for Gamma-Ray Bursts". Astrophysical Journal Letters . 392: L9. Bibcode:1992ApJ...392L...9D. doi:10.1086/186413.
  4. 1 2 3 4 5 Kouveliotou, C.; Duncan, R. C.; Thompson, C. (February 2003). "Magnetars". Scientific American ; Page 41.
  5. ↑ Thompson, Christopher; Duncan, Robert C. (July 1995). "The soft gamma repeaters as very strongly magnetized neutron stars - I. radiative mechanisms for outbursts". Monthly Notices of the Royal Astronomical Society. 275 (2): 255–300. Bibcode:1995MNRAS.275..255T. doi: 10.1093/mnras/275.2.255 .
  6. 1 2 3 4 "McGill SGR/AXP Online Catalog" . Retrieved 26 Jan 2021.
  7. ↑ Starr, Michelle (1 June 2020). "Astronomers Just Narrowed Down The Source of Those Powerful Radio Signals From Space". ScienceAlert.com. Retrieved 2 June 2020.
  8. 1 2 Kaspi, V. M. (April 2010). "Grand unification of neutron stars". Proceedings of the National Academy of Sciences. 107 (16). Proceedings of the National Academy of Sciences of the United States of America: 7147–7152. arXiv: 1005.0876 . Bibcode:2010PNAS..107.7147K. doi: 10.1073/pnas.1000812107 . PMC   2867699 . PMID   20404205.
  9. ↑ Condon, J. J. & Ransom, S. M. "Pulsar Properties (Essential radio Astronomy)". National Radio Astronomy Observatory. Retrieved 26 Feb 2021.
  10. 1 2 3 Kouveliotou, C.; Duncan, R. C.; Thompson, C. (February 2003). "Magnetars Archived 2007-06-11 at the Wayback Machine ". Scientific American ; Page 36.
  11. ↑ "HLD user program, at Dresden High Magnetic Field Laboratory" . Retrieved 2009-02-04.
  12. ↑ Naeye, Robert (February 18, 2005). "The Brightest Blast". Sky & Telescope . Retrieved 10 November 2020.
  13. ↑ Duncan, Robert. "'MAGNETARS', SOFT GAMMA REPEATERS & VERY STRONG MAGNETIC FIELDS". University of Texas.
  14. ↑ Wanjek, Christopher (February 18, 2005). "Cosmic Explosion Among the Brightest in Recorded History". NASA . Retrieved 17 December 2007.
  15. ↑ Dooling, Dave (May 20, 1998). ""Magnetar" discovery solves 19-year-old mystery". Science@NASA Headline News. Archived from the original on 14 December 2007. Retrieved 17 December 2007.
  16. ↑ Thompson, Christopher; Duncan, Robert C. (1993). "Neutron Star Dynamos and the Origins of Pulsar Magnetism". Astrophysical Journal. 408: 194–217. Bibcode:1993ApJ...408..194T. doi: 10.1086/172580 – via NASA Astrophysics Data System.
  17. ↑ Price, Daniel J.; Rosswog, Stephan (May 2006). "Producing Ultrastrong Magnetic Fields in Neutron Star Mergers". Science. 312 (5774): 719–722. arXiv: astro-ph/0603845 . Bibcode:2006Sci...312..719P. doi:10.1126/science.1125201. PMID   16574823. S2CID   30023248. Archived from the original on 2018-07-17. Retrieved 2012-07-13. Open Access logo PLoS transparent.svg
  18. ↑ Zhou, Ping; Vink, Jacco; Safi-Harb, Samar; Miceli, Marco (September 2019). "Spatially resolved X-ray study of supernova remnants that host magnetars: Implication of their fossil field origin". Astronomy & Astrophysics. 629 (A51): 12. arXiv: 1909.01922 . Bibcode:2019A&A...629A..51Z. doi:10.1051/0004-6361/201936002. S2CID   201252025. Open Access logo PLoS transparent.svg
  19. ↑ Kouveliotou, p.237
  20. ↑ Popov, S. B.; Prokhorov, M. E. (April 2006). "Progenitors with enhanced rotation and the origin of magnetars". Monthly Notices of the Royal Astronomical Society. 367 (2): 732–736. arXiv: astro-ph/0505406 . Bibcode:2006MNRAS.367..732P. doi: 10.1111/j.1365-2966.2005.09983.x . S2CID   14930432. Open Access logo PLoS transparent.svg
  21. ↑ Cline, T. L., Desai, U. D., Teegarden, B. J., Evans, W. D., Klebesadel, R. W., Laros, J. G. (Apr 1982). "Precise source location of the anomalous 1979 March 5 gamma-ray transient". The Astrophysical Journal. 255: L45–L48. Bibcode:1982ApJ...255L..45C. doi:10.1086/183766. hdl: 2060/19820012236 .{{cite journal}}: CS1 maint: multiple names: authors list (link) Open Access logo PLoS transparent.svg
  22. ↑ "Biggest Explosions in the Universe Powered by Strongest Magnets" . Retrieved 9 July 2015.
  23. ↑ Shainblum, Mark (21 February 2008). "Jekyll-Hyde neutron star discovered by researchers]". McGill University.
  24. 1 2 "The Hibernating Stellar Magnet: First Optically Active Magnetar-Candidate Discovered". ESO. 23 September 2008.
  25. ↑ "Magnetar discovered close to supernova remnant Kesteven 79". ESA/XMM-Newton/ Ping Zhou, Nanjing University, China. 1 September 2014.
  26. ↑ van Putten, Maurice H P M; Della Valle, Massimo (2018-09-04). "Observational evidence for extended emission to GW170817". Monthly Notices of the Royal Astronomical Society: Letters. 482 (1): L46–L49. arXiv: 1806.02165 . Bibcode:2019MNRAS.482L..46V. doi: 10.1093/mnrasl/sly166 . ISSN   1745-3925. S2CID   119216166.
  27. ↑ Timmer, John (4 November 2020). "We finally know what has been making fast radio bursts - Magnetars, a type of neutron star, can produce the previously enigmatic bursts". Ars Technica . Retrieved 4 November 2020.
  28. ↑ Cofield, Calla; Andreoli, Calire; Reddy, Francis (4 November 2020). "NASA Missions Help Pinpoint the Source of a Unique X-ray, Radio Burst". NASA . Retrieved 4 November 2020.
  29. ↑ Andersen, B.; et al. (4 November 2020). "A bright millisecond-duration radio burst from a Galactic magnetar". Nature . 587 (7832): 54–58. arXiv: 2005.10324 . Bibcode:2020Natur.587...54C. doi:10.1038/s41586-020-2863-y. PMID   33149292. S2CID   218763435 . Retrieved 5 November 2020.
  30. ↑ Drake, Nadia (5 May 2020). "'Magnetic Star' Radio Waves Could Solve the Mystery of Fast Radio Bursts - The surprise detection of a radio burst from a neutron star in our galaxy might reveal the origin of a bigger cosmological phenomenon". Scientific American . Retrieved 9 May 2020.
  31. ↑ Starr, Michelle (1 May 2020). "Exclusive: We Might Have First-Ever Detection of a Fast Radio Burst in Our Own Galaxy". ScienceAlert.com. Retrieved 9 May 2020.
  32. ↑ "Strange Ring Found Around Dead Star". Archived from the original on 2012-07-21.
  33. ↑ "NASA - European Satellites Probe a New Magnetar". www.nasa.gov.
  34. ↑ "Chandra :: Photo Album :: Westerlund 1 :: 02 Nov 05". chandra.harvard.edu.
  35. ↑ "Magnetar Formation Mystery Solved?". www.eso.org.
  36. ↑ Wood, Chris. "Very Large Telescope solves magnetar mystery" GizMag, 14 May 2014. Accessed: 18 May 2014.
  37. ↑ A new low-B magnetar
  38. ↑ Rea, N.; Viganò, D.; Israel, G. L.; Pons, J. A.; Torres, D. F. (2014-01-01). "3XMM J185246.6+003317: Another Low Magnetic Field Magnetar". The Astrophysical Journal Letters. 781 (1): L17. arXiv: 1311.3091 . Bibcode:2014ApJ...781L..17R. doi:10.1088/2041-8205/781/1/L17. hdl:10045/34971. ISSN   0004-637X. S2CID   118736623.
  39. ↑ "A Cosmic Baby Is Discovered, and It's Brilliant". NASA Jet Propulsion Laboratory (JPL).
  40. ↑ Harvard-Smithsonian Center for Astrophysics (8 January 2021). "Chandra observations reveal extraordinary magnetar". Phys.org . Retrieved 8 January 2021.
  41. ↑ Kasen, D.; L. Bildsten. (1 Jul 2010). "Supernova Light Curves Powered by Young Magnetars". Astrophysical Journal. 717 (1): 245–249. arXiv: 0911.0680 . Bibcode:2010ApJ...717..245K. doi:10.1088/0004-637X/717/1/245. S2CID   118630165.
  42. ↑ Woosley, S. (20 Aug 2010). "Bright Supernovae From Magnetar Birth". Astrophysical Journal Letters. 719 (2): L204–L207. arXiv: 0911.0698 . Bibcode:2010ApJ...719L.204W. doi:10.1088/2041-8205/719/2/L204. S2CID   118564100.
  43. ↑ Inserra, C.; Smartt, S. J.; Jerkstrand, A.; Valenti, S.; Fraser, M.; Wright, D.; Smith, K.; Chen, T.-W.; Kotak, R.; et al. (June 2013). "Super Luminous Ic Supernovae: catching a magnetar by the tail". The Astrophysical Journal. 770 (2): 128. arXiv: 1304.3320 . Bibcode:2013ApJ...770..128I. doi:10.1088/0004-637X/770/2/128. S2CID   13122542.
  44. ↑ Queen's University, Belfast (16 October 2013). "New light on star death: Super-luminous supernovae may be powered by magnetars". ScienceDaily . Retrieved 21 October 2013.
  45. ↑ M. Nicholl; S. J. Smartt; A. Jerkstrand; C. Inserra; M. McCrum; R. Kotak; M. Fraser; D. Wright; T.-W. Chen; K. Smith; D. R. Young; S. A. Sim; S. Valenti; D. A. Howell; F. Bresolin; R. P. Kudritzki; J. L. Tonry; M. E. Huber; A. Rest; A. Pastorello; L. Tomasella; E. Cappellaro; S. Benetti; S. Mattila; E. Kankare; T. Kangas; G. Leloudas; J. Sollerman; F. Taddia; E. Berger; R. Chornock; G. Narayan; C. W. Stubbs; R. J. Foley; R. Lunnan; A. Soderberg; N. Sanders; D. Milisavljevic; R. Margutti; R. P. Kirshner; N. Elias-Rosa; A. Morales-Garoffolo; S. Taubenberger; M. T. Botticella; S. Gezari; Y. Urata; S. Rodney; A. G. Riess; D. Scolnic; W. M. Wood-Vasey; W. S. Burgett; K. Chambers; H. A. Flewelling; E. A. Magnier; N. Kaiser; N. Metcalfe; J. Morgan; P. A. Price; W. Sweeney; C. Waters. (17 Oct 2013). "Slowly fading super-luminous supernovae that are not pair-instability explosions". Nature. 7471. 502 (346): 346–9. arXiv: 1310.4446 . Bibcode:2013Natur.502..346N. doi:10.1038/nature12569. PMID   24132291. S2CID   4472977.

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