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Berger, Johannes

doi:10.1007/978-3-658-04853-2_5

Cited by 257 publications

(425 citation statements)

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“…Indeed, it is important to note that millisecond magnetars are not the only viable explanation for X-ray afterglow curves (Berger 2014). In fact, the standard interpretation involves the GRB jet interacting with the surrounding interstellar medium (culminating in a fireball), which produces multi-band emission (Mészáros & Rees 1993).…”

Section: Discussionmentioning

confidence: 99%

“…GRB 090510 is a short GRB at redshift z = 0.9 (Ackermann et al 2010), with prompt emission duration T 90 = 0.3 ± 0.1 s in the 15 − 350 keV band and photon index Γ ≈ 0.98. As this object was likely born out of a merger event (Berger 2014), we assume the star is more compact, and take values R = 12 km and M = 2.0M . For this GRB, no impulsive-fireball phase is explicitly evident in the Swift-XRT data, though a plateau is seen at early times, eventually decaying as ∼ t −2 (Evans et al 2009).…”

Section: A Short Grb: 090510mentioning

confidence: 99%

“…A common feature of gamma-ray bursts (GRBs) is the emergence of a shallow decay phase following the prompt emission (Nousek et al 2006). The absence of spectral evolution during this 'plateau' suggests that the afterglow is powered by continuous energy injections from a long-lived remnant (Zhang et al 2006), born out of gravitational collapse or a compact object merger (Piran 2004;Berger 2014). Depending on the properties of the progenitor star(s), a remnant in the form of a rapidly rotating, highly-magnetised neutron star ('millisecond magnetar') is expected.…”

Section: Introductionmentioning

confidence: 99%

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Evidence for Magnetar Precession in X-Ray Afterglows of Gamma-Ray Bursts

Suvorov

Kokkotas

2020

ApJL

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Many gamma-ray bursts are followed by periods of extended emission. At least in some cases, the burst afterglow may be powered by a rapidly rotating, highly-magnetised neutron star, which spins down due to electromagnetic and gravitational wave emission. Such a remnant is likely to strongly precess in the early stages of its life, which would lead to modulations in the X-ray luminosity as the triaxiality of the system evolves over time. Using a radiation profile appropriate for a precessing, oblique rotator, we find that Swift-XRT data of a long (080602) and a short (090510) burst matches the model with significantly higher accuracy (mean-square residuals dropping by 200% in the early stages of the extended emission) than for an orthogonal rotator. We interpret this as evidence for precession in newborn magnetars.

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Section: Discussionmentioning

confidence: 99%

Section: A Short Grb: 090510mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Evidence for Magnetar Precession in X-Ray Afterglows of Gamma-Ray Bursts

Suvorov

Kokkotas

2020

ApJL

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“…Merging DNS and NS+BH binaries are considered the most promising sources to explain the phenomenology of short GRBs (Paczynski 1986;Eichler et al 1989;Narayan et al 1992;Fox et al 2005;Rezzolla et al 2011;Berger 2014).…”

Section: Short Grbsmentioning

confidence: 99%

Formation of Double Neutron Star Systems

Tauris

Krämer

Freire

et al. 2017

ApJ

619

690

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Double neutron star (DNS) systems represent extreme physical objects and the endpoint of an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems and their mergers are anticipated to be discovered using the Square-Kilometre-Array searching for radio pulsars and high-frequency gravitational wave detectors (LIGO/VIRGO), respectively. Here we discuss all key properties of DNS systems, as well as selection effects, and combine the latest observational data with new theoretical progress on various physical processes with the aim of advancing our knowledge on their formation. We examine key interactions of their progenitor systems and evaluate their accretion history during the high-mass X-ray binary stage, the common envelope phase and the subsequent Case BB mass transfer, and argue that the first-formed NSs have accreted at most ∼ 0.02 M ⊙ . We investigate DNS masses, spins and velocities, and in particular correlations between spin period, orbital period and eccentricity. Numerous Monte Carlo simulations of the second supernova (SN) events are performed to extrapolate pre-SN stellar properties and probe the explosions. All known close-orbit DNS systems are consistent with ultra-stripped exploding stars. Although their resulting NS kicks are often small, we demonstrate a large spread in kick magnitudes which may, in general, depend on the past interaction history of the exploding star and thus correlate with the NS mass. We analyze and discuss NS kick directions based on our SN simulations. Finally, we discuss the terminal evolution of close-orbit DNS systems until they merge and possibly produce a short γ-ray burst.

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“…Recently, three FRBs (FRBs 180924, 181112 and 190523) that have not yet been observed to repeat are localized (Bannister et al 2019;Ravi et al 2019;. The host galaxies of these three FRBs are massive galaxies with little star formation, which are similar to those of short gamma-ray bursts (Berger 2014). Moreover, the offsets between the bursts and host centers are about 4 kpc and 29 kpc for FRB 180924 and FRB 190523, respectively.…”

Section: Introductionmentioning

confidence: 99%

The Rarity of Repeating Fast Radio Bursts from Binary Neutron Star Mergers

Zhang

Wang

2020

ApJ

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Fast radio bursts (FRBs) are extragalactic, bright pulses of emission at radio frequency with milliseconds duration. Observationally, FRBs can be divided into two classes, repeating FRBs and non-repeating FRBs. At present, twenty repeating FRBs have been discovered with unknown physical origins. Localization of the first repeating FRB 121102 and discovery of an associated persistent radio source support that FRBs are powered by young millisecond magnetars, which could be formed by core-collapses of massive stars or binary neutron stars mergers. These two formation channels can be distinguished by gravitational waves generated by binary neutron stars mergers. We first calculate the lower limit of the local formation rate of repeating FRBs observed by the Canadian Hydrogen Intensity Mapping Experiment (CHIME) . Then we show that only a small fraction (6%) of repeating FRBs is produced by young magnetars from binary neutron star mergers, basing on the gravitational wave detections by the third observing run (O3) of Advanced LIGO/Virgo gravitational-wave detectors. Therefore, we believe that repeating FRBs are more likely produced by the magnetars newborn from the core-collapses of massive stars rather than the magnetars from the binary neutron stars mergers.

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Zukunftsperspektiven

Cited by 257 publications

References 0 publications

Evidence for Magnetar Precession in X-Ray Afterglows of Gamma-Ray Bursts

Evidence for Magnetar Precession in X-Ray Afterglows of Gamma-Ray Bursts

Formation of Double Neutron Star Systems

The Rarity of Repeating Fast Radio Bursts from Binary Neutron Star Mergers

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