REVISITING THE LONG/SOFT-SHORT/HARD CLASSIFICATION OF GAMMA-RAY BURSTS IN THE<i>FERMI</i>ERA

Zhang, Fu-Wen; Shao, L.; Yan, Jing-Zhi; Wei, Da-Ming

doi:10.1088/0004-637x/750/2/88

Cited by 98 publications

(103 citation statements)

References 65 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Most remarkable is that this model gives the theoretical explanation for the fulfillment of the E p,i -E iso relation for the short bursts (see Fig. 8 and Zhang et al 2012;Calderone et al 2015;Ruffini et al 2015b).…”

Section: Theoretical Interpretation Of S-grbs Within the Ns-ns Mergermentioning

confidence: 61%

See 1 more Smart Citation

ON THE CLASSIFICATION OF GRBs AND THEIR OCCURRENCE RATES

Ruffini

Rueda

Muccino

et al. 2016

ApJ

238

View full text Add to dashboard Cite

There is mounting evidence for the binary nature of the progenitors of gamma-ray bursts (GRBs). For a long GRB, the induced gravitational collapse (IGC) paradigm proposes as progenitor, or "in-state", a tight binary system composed of a carbon-oxygen core (CO core ) undergoing a supernova (SN) explosion which triggers hypercritical accretion onto a neutron star (NS) companion. For a short GRB, a NS-NS merger is traditionally adopted as the progenitor. We divide long and short GRBs into two sub-classes, depending on whether or not a black hole (BH) is formed in the merger or in the hypercritical accretion process exceeding the NS critical mass. For long bursts, when no BH is formed we have the sub-class of X-ray flashes (XRFs), with isotropic energy E iso 10 52 erg and rest-frame spectral peak energy E p,i 200 keV. When a BH is formed we have the sub-class of binary-driven hypernovae (BdHNe), with E iso 10 52 erg and E p,i 200 keV. In analogy, short bursts are similarly divided into two sub-classes. When no BH is formed, short gamma-ray flashes (S-GRFs) occur, with E iso 10 52 erg and E p,i 2 MeV. When a BH is formed, the authentic short GRBs (S-GRBs) occur, with E iso 10 52 erg and E p,i 2 MeV. We give examples and observational signatures of these four sub-classes and their rate of occurrence. From their respective rates it is possible that "in-states" of S-GRFs and S-GRBs originate from the "out-states" of XRFs. We indicate two additional progenitor systems: white dwarf-NS and BH-NS. These systems have hybrid features between long and short bursts. In the case of S-GRBs and BdHNe evidence is given of the coincidence of the onset of the high energy GeV emission with the birth of a Kerr BH.

show abstract

Section: Theoretical Interpretation Of S-grbs Within the Ns-ns Mergermentioning

confidence: 61%

“…8 and Zhang et al 2012;Muccino et al 2013;Calderone et al 2015;Ruffini et al 2015b) and increase monotonically with E iso .…”

Section: General Propertiesmentioning

confidence: 83%

ON THE CLASSIFICATION OF GRBs AND THEIR OCCURRENCE RATES

Ruffini

Rueda

Muccino

et al. 2016

ApJ

238

View full text Add to dashboard Cite

show abstract

“…The Amati correlation was investigated (Basak & Rao 2013;Gruber 2012) and a link between short and long GRBs was discovered (Muccino et al 2013). It gave insight into the GRB afterglow population (Racusin et al 2011), allowed to observe a number of high-energy GRBs (with photon energies exceeding 100 MeV, or even 10 GeV) (Atwood et al 2013), and provided a verification of the short-long classification (Zhang et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Distinguishing short and longFermigamma-ray bursts

Tarnopolski

2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Two classes of gamma-ray bursts (GRBs), short and long, have been determined without any doubts, and are usually ascribed to different progenitors, yet these classes overlap for a variety of descriptive parameters. A subsample of 46 long and 22 short Fermi GRBs with estimated Hurst Exponents (HEs), complemented by minimum variability time-scales (MVTS) and durations (T 90 ) is used to perform a supervised Machine Learning (ML) and Monte Carlo (MC) simulation using a Support Vector Machine (SVM) algorithm. It is found that while T 90 itself performs very well in distinguishing short and long GRBs, the overall success ratio is higher when the training set is complemented by MVTS and HE. These results may allow to introduce a new (non-linear) parameter that might provide less ambiguous classification of GRBs.

show abstract

“…The division line between the long-duration GRBs (LGRBs) and short-duration GRBs (SGRBs) is around 2 seconds in the BATSE 50 − 300 keV band. Although the significance of this bimodality and the division line depend on the sensitivity and energy band of the detectors (Richardson et al 1996;Bissaldi et al 2011;Zhang et al 2012;Qin et al 2013), the authenticity of the bimodal T 90 distribution is confirmed not only with a larger BATSE sample (Meegan et al 1996;Paciesas et al 1999), but also by GRB data collected from other instruments such as BeppoSAX ), INTEGRAL Savchenko et al 2012;Bošnjak et al 2014), Swift and Fermi (Paciesas et al 2012;von Kienlin et al 2014). The existence of two phenomenological classes of GRBs is firmly established.…”

Section: Introductionmentioning

confidence: 97%

A Comparative Study of Long and Short Grbs. I. Overlapping Properties

Li¹,

Zhang²,

Lü³

2016

ApJS

View full text Add to dashboard Cite

Gamma ray bursts (GRBs) are classified into long and short categories based on their durations. Broad band studies suggest that these two categories of objects roughly correspond to two different classes of progenitor systems, i.e. compact star mergers (Type I) vs. massive star core collapse (Type II). However, the duration criterion sometimes leads to mis-identification of the progenitor systems. We perform a comprehensive multi-wavelength comparative study between duration-defined long GRBs and short GRBs as well as the so-called "consensus" long GRBs and short GRBs (which are believed to be more closely related to the two types of progenitor systems). The parameters we study include two parts: the prompt emission properties including duration (T 90 ), spectral peak energy (E p ), low energy photon index (α), isotropic γ-ray energy (E γ,iso ), isotropic peak luminosity (L p,iso ), and the amplitude parameters (f and f eff ); and the host galaxy properties including stellar mass (M * ), star formation rate (SFR), metallicity ([X/H]), half light radius (R 50 ), angular and physical (R off ) offset of the afterglow from the center of the host galaxy, the normalized offset (r off = R off /R 50 ), and the brightness fraction F light . For most parameters, we find interesting overlapping properties between the two populations in both 1D and 2D distribution plots. The three best parameters for the classification purpose are T 90 , f eff , and F light . However, no single parameter alone is good enough to place a particular burst into the right physical category, suggesting a need of multiple criteria for physical classification.

show abstract

REVISITING THE LONG/SOFT-SHORT/HARD CLASSIFICATION OF GAMMA-RAY BURSTS IN THEFERMIERA

Cited by 98 publications

References 65 publications

ON THE CLASSIFICATION OF GRBs AND THEIR OCCURRENCE RATES

ON THE CLASSIFICATION OF GRBs AND THEIR OCCURRENCE RATES

Distinguishing short and longFermigamma-ray bursts

A Comparative Study of Long and Short Grbs. I. Overlapping Properties

Contact Info

Product

Resources

About