AD 775 pulse of cosmogenic radionuclides production as imprint of a Galactic gamma-ray burst

Павлов, А. А.; Blinov, A. V.; Konstantinov, A. N.; Ostryakov, V. M.; Vasilyev, G. I.; Vdovina, M. A.; Волков, П. А.

doi:10.1093/mnras/stt1468

Cited by 62 publications

(88 citation statements)

References 34 publications

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“…775 AD was analyzed using biennial 14 C data by Miyake et al (2012), who suggested that the event was probably caused by γ -rays from an unknown nearby supernova. This event is confirmed by annual 14 C data from a German oak tree , Russian and American tree samples (Jull et al 2014), New Zealand trees (Güttler et al 2013), etc., and corals from the Chinese Sea (Liu et al 2014) According to model simulations, the production of 14 C appears in agreement with that of 10 Be Melott and Thomas 2012;Pavlov et al 2013). Although some exotic scenarios were proposed for the event: an unidentified nearby supernova ); a gamma-ray burst (Hambaryan and Neuhäuser 2013;Pavlov et al 2013); or even a cometary impact on Earth (Liu et al 2014), it is generally accepted now that it was a signature of a (probably, consequence of) extreme SEP event Eichler and Mordecai 2012;Usoskin et al 2013;Melott and Thomas 2012;Thomas et al 2013;Cliver et al 2014).…”

Section: The Event Of 775 Ad: the Worst Case Scenario?mentioning

confidence: 82%

A history of solar activity over millennia

Usoskin

2017

Living Rev Sol Phys

391

241

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Presented here is a review of present knowledge of the long-term behavior of solar activity on a multi-millennial timescale, as reconstructed using the indirect proxy method. The concept of solar activity is discussed along with an overview of the special indices used to quantify different aspects of variable solar activity, with special emphasis upon sunspot number. Over long timescales, quantitative information about past solar activity can only be obtained using a method based upon indirect proxies, such as the cosmogenic isotopes 14 C and 10 Be in natural stratified archives (e.g., tree rings or ice cores). We give an historical overview of the development of the proxy-based method for past solar-activity reconstruction over millennia, as well as a description of the modern state. Special attention is paid to the verification and cross-calibration of reconstructions. It is argued that this method of cosmogenic isotopes makes a solid basis for studies of solar variability in the past on a long timescale (centuries to millennia) during the Holocene. A separate section is devoted to reconstructions of strong solar energetic-particle (SEP) events in the past, that suggest that the present-day average SEP flux is broadly consistent with estimates on longer timescales, and that the occurrence of extra-strong events is unlikely. Finally, the main features of the long-term evolution of solar magnetic activity, including the

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Section: The Event Of 775 Ad: the Worst Case Scenario?mentioning

confidence: 82%

A history of solar activity over millennia

Usoskin

2017

Living Rev Sol Phys

391

241

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“…The non-solar sources include a supernova hidden behind a dust cloud (Allen 2012) and galactic short-duration (Hambaryan & Neuhäuser 2013) and long-duration gamma-ray bursts (Pavlov et al 2013). Melott & Thomas (2012) and Usoskin et al (2013) favor a standard (eruptive flare; Reames 2013) solar source, and Eichler & Mordecai (2012) proposed a non-traditional solar source-a superflare caused by a large comet colliding with the Sun.…”

Section: Introductionmentioning

confidence: 99%

On a Solar Origin for the Cosmogenic Nuclide Event of 775 A.D.

Cliver

Tylka

Dietrich

et al. 2014

ApJ

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We explore requirements for a solar particle event (SPE) and flare capable of producing the cosmogenic nuclide event of 775 a.d., and review solar circumstances at that time. A solar source for 775 would require a >1 GV spectrum ∼45 times stronger than that of the intense high-energy SPE of 1956 February 23. This implies a >30 MeV proton fluence (F 30 ) of ∼8 × 10 10 proton cm −2 , ∼10 times larger than that of the strongest 3 month interval of SPE activity in the modern era. This inferred F 30 value for the 775 SPE is inconsistent with the occurrence probability distribution for >30 MeV solar proton events. The best guess value for the soft X-ray classification (total energy) of an associated flare is ∼X230 (∼9 × 10 33 erg). For comparison, the flares on 2003 November 4 and 1859 September 1 had observed/inferred values of ∼X35 (∼10 33 erg) and ∼X45 (∼2 × 10 33 erg), respectively. The estimated size of the source active region for a ∼10 34 erg flare is ∼2.5 times that of the largest region yet recorded. The 775 event occurred during a period of relatively low solar activity, with a peak smoothed amplitude about half that of the second half of the 20th century. The ∼1945-1995 interval, the most active of the last ∼2000 yr, failed to witness a SPE comparable to that required for the proposed solar event in 775. These considerations challenge a recent suggestion that the 775 event is likely of solar origin.

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“…The considerations of Cliver et al [11] challenge a suggestion that the 775 event is likely of solar origin. This event could originate from high-energy irradiation of the atmosphere by a Galactic gamma-ray burst [13]. A solar source for the AD 775 event would require the proton fluence F(>30 MeV) = 8 ·10 10 cm −2 , 10 times larger than that of the strongest 3 month interval of SPE activity in the modern era.…”

Section: Discussion: Ultimate Fluxes and Fluencesmentioning

confidence: 99%

Ultimate Spectrum of Solar/Stellar Cosmic Rays

Struminsky¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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We propose a physical approach to reconstruct the ultimate spectrum of solar/stellar cosmic rays (SCR) in a given point in the heliosphere (stellar sphere) basing on maximal value of magnetic field strength in active region and its characteristic linear dimension. An accelerator of given dimensions and magnetic field strength may accelerate to some finite energy for a given time (a maximal energy of SCR). We use the spectrum of SCR proposed by Syrovatsky (1961) for relativistic and non-relativistic energies normalizing it to galactic cosmic ray (GCR) intensity at the maximal SCR energy. Maximal values of SCR flux propagating in the heliosphere are determined by equilibrium between pressure of interplanetary magnetic field and dynamic pressure of SCR (Freier and Webber, 1963). We use the characteristic time of fluence accumulation obtained from the observations to derive the ultimate fluence of a single solar proton event (SPE). Our estimates are consisted with the observational upper limits on the strength of SPEs on the timescale of tens of millennia (Usoskin and Kovaltsov, 2012) and during the most active interval of 1945 -1995 during the last 2000 years . The obtained numbers of >30 MeV and >200 MeV solar protons for a single proton event is not enough to explain the extreme particle event occurred in about 775 AD, a sequence of about twenty proton events may explain it. An extension of the model to cases of stellar flares is discussed.

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AD 775 pulse of cosmogenic radionuclides production as imprint of a Galactic gamma-ray burst

Cited by 62 publications

References 34 publications

A history of solar activity over millennia

A history of solar activity over millennia

On a Solar Origin for the Cosmogenic Nuclide Event of 775 A.D.

Ultimate Spectrum of Solar/Stellar Cosmic Rays

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