FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2094464523> ?p ?o ?g. }

• W2094464523 endingPage "1005" @default.
• W2094464523 startingPage "980" @default.
• W2094464523 abstract "The extraordinary 1998 August 27 giant flare places strong constraints on the physical properties of its source, SGR 1900+14. We make detailed comparisons of the published data with the magnetar model, which identifies the soft gamma repeaters as neutron stars endowed with ~1015 G magnetic fields. The giant flare evolved through three stages, whose radiative mechanisms we address in turn. The extreme peak luminosity L > 106LEdd, hard spectrum, and rapid variability of the initial ~0.5 s spike emission all point to an expanding pair fireball with very low baryon contamination. We argue that this energy must have been deposited directly through shearing and reconnection of a magnetar-strength external magnetic field. Low-order torsional oscillations of the star fail to transmit energy rapidly enough to the exterior, if the surface field is much weaker. A triggering mechanism is proposed, whereby a helical distortion of the core magnetic field induces large-scale fracturing in the crust and a twisting deformation of the crust and exterior magnetic field. After the initial spike (whose ~0.4 s duration can be related to the Alfvén crossing time of the core), very hot (T ≲ 1 MeV) plasma rich in electron-positron pairs remains confined close to the star on closed magnetic field lines. The envelope of the August 27 flare can be accurately fitted, after ~40 s, by the contracting surface of such a trapped fireball. The form of this fit gives evidence that the temperature of the trapped pair plasma decreases outward from its center. We quantify the effects of direct neutrino pair emission on the X-ray light curve, thereby deducing a lower bound μmin ~ 1 × 1032 G cm3 to the magnetic moment of the confining field, comparable to the strongest fields measured in radio pulsars. The radiative flux during the intermediate ~40 s of the burst appears to exceed the trapped fireball fit. The lack of strong rotational modulation and intermediate hardness of this smooth tail are consistent with the emission from an extended pair corona, in which O-mode photons are heated by Compton scattering. This feature could represent residual seismic activity within the star and accounts for ~10% of the total flare fluence. We consider in detail the critical luminosity, below which a stable balance can be maintained between heating and radiative cooling in a confined, magnetized pair plasma, but above which the confined plasma runs away to a trapped fireball in LTE. The emergence of large-amplitude pulsations at ~40 s probably represents a transition to a pair-depleted photosphere whose main source of opacity is electrons (and ions) ablated from the heated neutron star surface. The best-fit temperature of the blackbody component of the spectrum equilibrates at a value that agrees well with the regulating effect of photon splitting. The remarkable four-peaked substructure within each 5.16 s pulse, as well as the corresponding collimation of the X-ray flux, has a simple explanation based on the strong inequality between the scattering cross sections of the two photon polarization modes. The width of each X-ray jet is directly related to the amount of matter advected outward by the high cross section ordinary mode." @default.
• W2094464523 created "2016-06-24" @default.
• W2094464523 creator A5006526357 @default.
• W2094464523 creator A5029794318 @default.
• W2094464523 date "2001-11-10" @default.
• W2094464523 modified "2023-10-12" @default.
• W2094464523 title "The Giant Flare of 1998 August 27 from SGR 1900+14. II. Radiative Mechanism and Physical Constraints on the Source" @default.
• W2094464523 cites W1537744696 @default.
• W2094464523 cites W1576734198 @default.
• W2094464523 cites W1621932864 @default.
• W2094464523 cites W1675800434 @default.
• W2094464523 cites W1966164576 @default.
• W2094464523 cites W1967825921 @default.
• W2094464523 cites W1969499378 @default.
• W2094464523 cites W1970857837 @default.
• W2094464523 cites W1971127307 @default.
• W2094464523 cites W1972035771 @default.
• W2094464523 cites W1978505636 @default.
• W2094464523 cites W1979575263 @default.
• W2094464523 cites W1981143544 @default.
• W2094464523 cites W1986515303 @default.
• W2094464523 cites W2008425255 @default.
• W2094464523 cites W2010755947 @default.
• W2094464523 cites W2013277967 @default.
• W2094464523 cites W2014700299 @default.
• W2094464523 cites W2016006324 @default.
• W2094464523 cites W2017072609 @default.
• W2094464523 cites W2018144815 @default.
• W2094464523 cites W2018151163 @default.
• W2094464523 cites W2021443138 @default.
• W2094464523 cites W2026894175 @default.
• W2094464523 cites W2032779991 @default.
• W2094464523 cites W2033815590 @default.
• W2094464523 cites W2035391277 @default.
• W2094464523 cites W2038858559 @default.
• W2094464523 cites W2040451033 @default.
• W2094464523 cites W2041001575 @default.
• W2094464523 cites W2044792312 @default.
• W2094464523 cites W2046960399 @default.
• W2094464523 cites W2048469808 @default.
• W2094464523 cites W2048938903 @default.
• W2094464523 cites W2049710884 @default.
• W2094464523 cites W2056583859 @default.
• W2094464523 cites W2057983548 @default.
• W2094464523 cites W2060176052 @default.
• W2094464523 cites W2064826966 @default.
• W2094464523 cites W2065179406 @default.
• W2094464523 cites W2066552792 @default.
• W2094464523 cites W2068959108 @default.
• W2094464523 cites W2070650982 @default.
• W2094464523 cites W2074377846 @default.
• W2094464523 cites W2074794433 @default.
• W2094464523 cites W2079476663 @default.
• W2094464523 cites W2080495687 @default.
• W2094464523 cites W2082482299 @default.
• W2094464523 cites W2085339226 @default.
• W2094464523 cites W2086329925 @default.
• W2094464523 cites W2091009532 @default.
• W2094464523 cites W2091313340 @default.
• W2094464523 cites W2106044341 @default.
• W2094464523 cites W2115517418 @default.
• W2094464523 cites W2122598746 @default.
• W2094464523 cites W2125521213 @default.
• W2094464523 cites W2128750553 @default.
• W2094464523 cites W2138712210 @default.
• W2094464523 cites W2169210246 @default.
• W2094464523 cites W2569341887 @default.
• W2094464523 cites W3098498894 @default.
• W2094464523 cites W3101403501 @default.
• W2094464523 cites W3102425118 @default.
• W2094464523 cites W3103169171 @default.
• W2094464523 cites W3104328954 @default.
• W2094464523 cites W3106024263 @default.
• W2094464523 cites W3106163434 @default.
• W2094464523 cites W3125710173 @default.
• W2094464523 cites W3125973091 @default.
• W2094464523 doi "https://doi.org/10.1086/323256" @default.
• W2094464523 hasPublicationYear "2001" @default.
• W2094464523 type Work @default.
• W2094464523 sameAs 2094464523 @default.
• W2094464523 citedByCount "291" @default.
• W2094464523 countsByYear W20944645232012 @default.
• W2094464523 countsByYear W20944645232013 @default.
• W2094464523 countsByYear W20944645232014 @default.
• W2094464523 countsByYear W20944645232015 @default.
• W2094464523 countsByYear W20944645232016 @default.
• W2094464523 countsByYear W20944645232017 @default.
• W2094464523 countsByYear W20944645232018 @default.
• W2094464523 countsByYear W20944645232019 @default.
• W2094464523 countsByYear W20944645232020 @default.
• W2094464523 countsByYear W20944645232021 @default.
• W2094464523 countsByYear W20944645232022 @default.
• W2094464523 countsByYear W20944645232023 @default.
• W2094464523 crossrefType "journal-article" @default.
• W2094464523 hasAuthorship W2094464523A5006526357 @default.
• W2094464523 hasAuthorship W2094464523A5029794318 @default.
• W2094464523 hasBestOaLocation W20944645231 @default.
• W2094464523 hasConcept C115260700 @default.

• next