Neutrino-heated winds from rotating protomagnetars

Vlasov, Andrey; Metzger, Brian D.; Thompson, Todd A.

doi:10.1093/mnras/stu1667

Cited by 41 publications

(44 citation statements)

References 83 publications

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“…Other estimates of r-process material production yield ≈ 0.01M ⊙ for a SN magnetized driven jet (Nishimura et al 2015) and 0.01M ⊙ for a magnetized neutrino-driven wind (Vlasov et al 2014). Since these processes require rapid rotation, and hence low metallicity, these authors estimate that the rate of such events is low compared to regular SNe.…”

Section: +76mentioning

confidence: 96%

“…However, the low rate can be consistent with a peculiar astrophysical explosion associated with a core collapse of massive stars. For instance, a magnetically powered outflow from newly born magnetars has been proposed as the site of the r-process nucleosynthesis (Suzuki & Nagataki 2005;Metzger et al 2008;Winteler et al 2012;Vlasov et al 2014;Nishimura et al 2015;Mösta et al 2015). This could happen in a peculiar SN (e.g.…”

Section: Peculiar Core-collapse Supernovaementioning

confidence: 99%

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r-PROCESS PRODUCTION SITES AS INFERRED FROM Eu ABUNDANCES IN DWARF GALAXIES

Beniamini

Hotokezaka

Piran

2016

ApJ

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Recent observations of r-process material in ultra-faint dwarf galaxies (UFDs) shed light on the sources of these elements. Strong upper limits on the Eu mass in some UFDs combined with detections of much larger masses in a UFD, Reticulum II, and other dwarf galaxies imply that Eu production is dominated by rare events, and that the minimal Eu mass observed in any UFD is approximately the amount of Eu mass produced per event. This is consistent with other independent observations in the Galaxy. We estimate, using a model independent likelihood analysis, the rate and Eu (Fe) mass produced per r-process (Fe production) event in dwarf galaxies including classical dwarfs and UFDs. The mass and rate of the Fe production events are consistent with the normal core-collapse supernova (ccSN) scenario. The Eu mass per event is 3 × 10 −5 M ⊙

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Section: +76mentioning

confidence: 96%

Section: Peculiar Core-collapse Supernovaementioning

confidence: 99%

r-PROCESS PRODUCTION SITES AS INFERRED FROM Eu ABUNDANCES IN DWARF GALAXIES

Beniamini

Hotokezaka

Piran

2016

ApJ

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“…If the PNS has a strong magnetic field and rotates rapidly, the magnetic force is important for the dynamics of the wind and for the thermal history of the fluid element (Metzger et al 2007;Vlasov et al 2014). In Metzger et al (2007), the criterion for which the wind is magnetically driven is shown (see their discussion above Equation (17) in their paper).…”

Section: The Effect Of the Rotation And The Magnetic Field Of The Pnsmentioning

confidence: 99%

Nucleosynthesis in Neutrino-Driven Winds in Hypernovae

Fujibayashi

Yoshida

Sekiguchi

2015

ApJ

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We investigate the nucleosynthesis in the neutrino-driven winds blown off from a  M 3 massive proto-neutron star (mPNS) temporarily formed during the collapse of a  M 100 star. Such mPNSs would be formed in hypernovae. We construct steady and spherically symmetric wind solutions. We set large neutrino luminosities of~-10 erg s 53 1and average energies of electron neutrinos and antineutrinos in the ranges of  = based on a recent numerical relativity simulation. The wind solutions indicate a temperaturedecrease timescale much shorter than that of the winds from ordinary PNSs, and, depending on  n , the winds can be both neutron-rich and proton-rich. In the neutron-rich wind, the r-process occurs and the abundance distribution of a fiducial wind model of the mPNS gives an approximate agreement with the abundance pattern of metal-poor weak r star HD 122563, although the third-peak elements are produced only when the n ē energy is much larger than the n e energy. In the proton-rich wind, the strong np-process occurs and > A 100 nuclides are synthesized. The synthesized nuclei can be neutron-rich in some cases because the large neutrino luminosity of the mPNS supplies a sufficient amount of neutrons.

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“…Even if baryon loading were to cease abruptly, a minimum time would be required to clear the jet of baryons, which we estimate to be t d ∼ 0.01 s as the dynamical timescale near the base of the wind (Ref. [36], Fig. 9).…”

mentioning

confidence: 92%

Quark deconfinement and the duration of short gamma-ray bursts

et al. 2016

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We propose a model for short duration gamma-ray bursts (sGRBs) based on the formation of a quark star after the merger of two neutron stars. We assume that the sGRB central engine is a proto-magnetar, which has been previously invoked to explain the plateau-like X-ray emission observed following both long and short GRBs. Here, we show that: i) a few milliseconds after the merger it is possible to form a stable and massive star made in part of quarks; ii) during the early cooling phase of the incompletely formed quark star, the flux of baryons ablated from the surface by neutrinos is large and it does not allow the outflow to achieve a bulk Lorentz factor high enough to produce a GRB; iii) after the quark burning front reaches the stellar surface, baryon ablation ceases and the jet becomes too baryon poor to produce a GRB; iv) however, between these two phases a GRB can be produced over the finite timescale required for the baryon pollution to cease; a characteristic timescale of the order of ∼ 0.1 s naturally results from the time the conversion front needs to cover the distance between the rotational pole and the latitude of the last closed magnetic field line; v) we predict a correlation between the luminosity of the sGRB and its duration, consistent with the data; vi) our model also predicts a delay of the order of ten seconds between the time of the merger event and the sGRB, allowing for the possibility of precursor emission and implying that the jet will encounter the dense cocoon formed immediately after the merger. Both long duration (lGRBs) and short duration Gamma Ray Bursts (sGRBs) start with a violent "prompt" emission phase, which generally lasts a few tens of seconds in the case of lGRBs and a few tenths of a second in sGRBs. The prompt emission is in many cases followed by some form of prolonged engine activity, commonly referred to as the "Quasi-Plateau" (QP) in the case of lGRBs and "Extended Emission" (EE) in the case of sGRBs [1]. Beyond similarities in their light curve behavior, sGRBs and lGRBs show remarkably similar spectral properties [2]. This led to the suggestion that a similar central engine is acting in both classes of GRBs, a sGRB being similar to a lGRB cut after 0.The progenitors of lGRBs and sGRBs, on the other hand, are believed to be quite different: the collapse of a massive star for long bursts [4] and the merger of two neutron stars (or of a neutron star and a black hole) for the short bursts [5]. In their original forms, both models postulated a hyper-accreting black hole as the source of the relativistic outflow powering the GRB. However, following the discovery of the prolonged emission, a new model for the engine has grown in popularity, based on the relativistic wind of a newly formed, rapidly rotating proto-magnetar [6,7]. The model was initially proposed to explain the structure of lGRBs, but more recently it has been adapted to interpret also sGRBs [8][9][10] [43].GRB prompt emission results from dissipation within a relativistic jet composed of electron-positron pai...

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Neutrino-heated winds from rotating protomagnetars

Cited by 41 publications

References 83 publications

r-PROCESS PRODUCTION SITES AS INFERRED FROM Eu ABUNDANCES IN DWARF GALAXIES

r-PROCESS PRODUCTION SITES AS INFERRED FROM Eu ABUNDANCES IN DWARF GALAXIES

Nucleosynthesis in Neutrino-Driven Winds in Hypernovae

Quark deconfinement and the duration of short gamma-ray bursts

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