Mini Review ARTICLE
Short Duration Gamma-Ray Bursts and Their Outflows in Light of GW170817
- Department of Physics, Oregon State University, Corvallis, OR, United States
The detection of GW170817, it’s extensive multi-wavelength follow-up campaign, and the large amount of theoretical development and interpretation that followed, have resulted in a significant step forward in the understanding of the binary neutron star merger phenomenon as a whole. One of its aspects is seeing the merger as a progenitor of short gamma-ray bursts (SGRB), which will be the subject of this review. On the one hand, GW170817 observations have confirmed some theoretical expectations, exemplified by the confirmation that binary neutron star mergers are the progenitors of SGRBs. In addition, the multimessenger nature of GW170817 has allowed for gathering of unprecedented data, such as the trigger time of the merger, the delay with which the gamma-ray photons were detected, and the brightening afterglow of an off-axis event. All together, the incomparable richness of the data from GW170817 has allowed us to paint a fairly detailed picture of at least one SGRB. I will detail what we learned, what new questions have arisen, and the perspectives for answering them when a sample of GW170817-comparable events have been studied.
Gamma-ray bursts (GRBs) are some of the most energetic explosions in the present day Universe, characterized by the release of large amounts of energy, within a few milliseconds to tens of seconds, resulting in the acceleration of relativistic outflows and the release of high-energy photons (Fishman and Meegan, 1995; Piran, 1999; Mészáros, 2002; Gehrels et al., 2009; Kumar and Zhang, 2015). They can be divided in at least two classes, based on the duration of their prompt phase, in which their emission is concentrated in the hard X-ray and gamma-ray bands and is characterized by fast variability (Kouveliotou et al., 1993). Long duration GRBs last 2 s or more, while short duration GRBs (SGRBs) last between a few milliseconds and 2 s. Alternative classifications have also been introduced, considering, e.g., short GRBs with extended emission (Norris and Bonnell, 2006; Dainotti et al., 2010; Norris et al., 2010; Barkov and Pozanenko, 2011; Dainotti et al., 2017), or attempting a more physical classification based on inferred progenitor properties (Lü et al., 2010; Bromberg et al., 2013).
In the last two and a half decades, the study of GRBs has concentrated on long duration GRBs, and a general consensus has grown around a model in which these events are associated with the collapse of the core of massive stars (Woosley and Bloom, 2006). While the collapse of most massive stars would ignite a core-collapse supernova, those that are fastly spinning and metal poor could also trigger a long duration GRB, powered by a compact central engine (Woosley, 1993; Woosley and Heger, 2006; Yoon et al., 2006). Whether the central engine is a fastly spinning, highly magnetized neutron star (NS) (Bucciantini et al., 2008; Bucciantini et al., 2009; Metzger et al., 2011) or an accreting black hole (BH) (Woosley, 1993; Lee et al., 2000; Lei et al., 2013) is the matter of open debate.
The interest on SGRBs had increased in the last decade, initially as a consequence of the launch of the Fermi satellite, which had a higher efficiency for detecting and localizing them compared to its predecessors (Meegan et al., 2009). More recently, the theoretical expectation that SGRBs had to be associated with the merger of binary NS systems (or, perhaps, system made by a BH and a NS) (Belczynski et al., 2006; Lee and Ramirez-Ruiz, 2007; Fong and Berger, 2013; Giacomazzo et al., 2013; Ruiz et al., 2016; Ciolfi, 2018) has made them the expected and highly anticipated high-frequency counterparts of gravitational wave sources (Nakar et al., 2006; Kiuchi et al., 2010; Schutz, 2011). Such expectations were supported by energetic and temporal arguments. Powering a GRB requires a large amount of energy, comparable to the rest mass of a stellar object converted to energy. In addition, said energy needs to be released in a matter of a fraction of a second, at least for SGRBs. Naked compact objects (NS and BH) are the only available candidates that can offer the required energy within a region of less than a light second. However, isolated NS and BH are unlikely progenitors, since some catastrophic event needs to take place to cause the sudden release of a large fraction of their total energy. Binary mergers are therefore a natural candidate, when at least one of the two members is a NS, since a binary BH system would merge in a bigger BH that would swallow all the matter and energy, instead of ejecting them as a relativistic outflow.1
All these expectations were confirmed by the detection of GW170817 (Abbott et al., 2017a) and its associated GRB GRB170817A (Abbott et al., 2017b; Goldstein et al., 2017; Savchenko et al., 2017; Zhang et al., 2018), afterglow, and kilonova (KN) (Abbott et al., 2017c; Abdalla et al., 2017; Alexander et al., 2017; Arcavi et al., 2017; Coulter et al., 2017; Cowperthwaite et al., 2017; Evans et al., 2017; Haggard et al., 2017; Hallinan et al., 2017; Kasen et al., 2017; Kim et al., 2017; Margutti et al., 2017; Pian et al., 2017; Siebert et al., 2017; Smartt et al., 2017; Soares-Santos et al., 2017; Tanvir et al., 2017; Troja et al., 2017; Valenti et al., 2017; D’Avanzo et al., 2018; Margutti et al., 2018; Mooley et al., 2018a; Mooley et al., 2018c; Lyman et al., 2018; Resmi et al., 2018; Villar et al., 2018; Ghirlanda et al., 2019; Lamb et al., 2019a). In this contribution I will review the key observations of GW170817 as a SGRB (also known as GRB170817A), the questions that were answered, and the new ones that were spurred, and briefly discuss what more insight is expected from the detection of more systems akin to GW170817 in future GW observing runs.
2 Before the Prompt Emission
In this Section 1 will review the physics of the SGRB outflow before the prompt emission phase begins, as it happened in GW170817. First of all, there is little doubt that the GW signal of GW170817 came from a binary compact merger, and that the masses of the two compact objects are compatible with being NS (Abbott et al., 2017a; Abbott et al., 2017b; Abbott et al., 2017c). The GW signal by itself does not allow to distinguish between NSs and BHs, but the richness of the electromagnetic signal that followed requires the presence of baryonic matter, and therefore at least one of the two components of the binary had to be a NS. Most likely they were both NSs (Coughlin and Dietrich, 2019).
2.1 The Time Delay
Besides the identification of the progenitor, a very important piece of information that GW170817 provided is the merger time, which allowed for the measuring of the time delay between the GWs and the gamma-ray signals. This delay, which we indicate as
• Engine Delay—While the time of the merger is the earliest time at which the jet from the central engine can be produced, there is the possibility of some delay (Cook et al., 1994; Lasota et al., 1996; Vietri and Stella, 1998; Ciolfi and Siegel, 2015). Such delay is difficult to predict theoretically but can be likely due either to the need of a transition in the engine itself or to the need of amplifying the magnetic field to a value large enough to launch a jet. The former can be quite long, up to years, and usually invokes a metastable, fastly spinning NS that collapses into a BH when its rotation period is increased by either internal or external torques. We indicate this delay time as
• Wind Delay—Owing to the detection of a KN and an off-axis SGRB from a structured outflow, we know that GW170817 ejected a non-relativistic wind. There can be a delay in launching such a wind as well, and we indicate it as
• Breakout delay—If the wind is ejected before the jet, then the jet has to propagate through the wind. The propagation happens at sub-relativistic speed, causing a delay of the head of the jet with respect to the GW signal that travels at the speed of light (Matzner, 2003; Morsony et al., 2007; Bromberg et al., 2011; Lazzati and Perna, 2019). We indicate the time it takes for the jet head to cross the wind as
• Photospheric delay—After the outflow has broken out of the leading edge of the wind, it needs to propagate out to the photospheric radius. At this point the jet becomes transparent and the necessary conditions for the release of the prompt gamma-ray radiation are met. We indicate the delay due to the propagation from the break out radius to the photospheric radius as
Dissipation delay—While at the photospheric radius the prompt emission can be radiated, it does not mean it is. In some models, such as the popular internal shock synchrotron model, the outflow needs to propagate out to the internal shock radius before the bulk energy of the flow is dissipated and turned into radiation. We indicate this additional delay as
FIGURE 1. The two possible timelines with all the phases that may contribute to the detected delay
For the first time, a measurement of the sum of all these possible delays was available for GW170817 (Abbott et al., 2017b). The prompt gamma-ray radiation was detected with a delay
The photospheric delay therefore had to contribute to a sizable part of the delay, since any other non-photospheric emission mechanism would require a longer delay (this allows to use the above equation to put a Lower limit on Γ (Beniamini 2020a). The wind delay, if there was any, had to be smaller than the jet delay, so that the jet-wind interaction could generate a structured outflow, as requested for modeling the afterglow emission. For the same reason, the jet delay itself could be fairly small but could not be null. Finally, the breakout and dissipation delays had to be small in order to accommodate the large expected photospheric delay. Note, however, that the prompt emission spectrum had a non-thermal shape, a property that is not expected form a simple photospheric emission model (see Section 3 for a more thorough discussion).
2.2 The Shaping of the Outflow
GW170817 was also the first GRB for which evidence of a structured outflow could be unequivocally determined. The structure of the outflow could be intrinsic, as the jet itself could have been launched with a non-uniform polar structure (Aloy et al., 2005; Kathirgamaraju et al., 2019). However, the relatively large energetics of GW170817 in gamma-rays and the shape of its afterglow lightcurve (see Section 4) suggest a wide structure, most likely brought about by the jet interaction with the wind from the merger (Lazzati and Perna, 2019; Salafia et al., 2020).
A typical SGRB jet with isotropic equivalent energy
3 The Prompt Emission
Approximately 1.75 s after the GW chirp, a gamma–ray pulse was observed by both the Fermi and INTEGRAL satellites from a position compatible with the direction from which the GWs arrived (Goldstein et al., 2017; Savchenko et al., 2017). The pulse was made by an initial spike of about half a second followed by a broader, less intense tail, for an overall duration of
The structured outflow model was successful at predicting that a SGRB would be detectable even at large off-axis angles (Lazzati et al., 2017a; Lazzati et al., 2017b). It correctly predicted the off-axis burst energetics and its duration. It could also successfully explain the detected delay between the GWs and the γ-rays. A comparison between the Fermi data and the bolometric photospheric emission (Lazzati et al., 2017b) is shown in the left panel of Figure 2. The one aspect of GW170817 that cannot be accounted for by the simple photospheric cocoon emission is the γ-ray spectrum of the prompt emission. At least in first approximation, the photosphere of an off-axis structured outflow is expected to produce a thermal pulse with temperature (Lazzati et al., 2017a; Lazzati et al., 2017b)
which would produce a spectrum peaked at a few KeV, in severe tension with the observed peak frequency at
FIGURE 2. Left panel (A): the prompt emission of GW170817. The blue step-line shows the Fermi data (Goldstein et al., 2017), while the orange solid line is the prediction from a theoretical simulation that assumes a structured outflow from the jet-wind interaction (Lazzati et al., 2017b). The radiation is assumed to be released at the photosphere. Right panel (B): Afterglow of GW170817. Symbols with error-bars show observations in the radio, optical, and X-ray bands. Solid lines show the best fit result for an afterglow model with a structured outflow and an observer located at
4 The Afterglow
The afterglow of GW170817 had its own share of unique features. To begin with, it was not detected for more then a week, until it was bright enough to be seen first in X-rays (Margutti et al., 2017; Troja et al., 2017) and, at around the two weeks mark, in radio waves (Hallinan et al., 2017; Troja et al., 2017). The detection of the afterglow at optical wavelengths had to wait for the dimming of the associated KN, and was performed only around day 110 with the Hubble Space Telescope (Lyman et al., 2018). Such late appearance of an afterglow is unprecedented, since the typical behavior is that the afterglow peaks very early, minutes to hours after the burst, and only dims with time afterward (van Paradijs et al., 2000; Nousek et al., 2006). A second unique feature of the afterglow of GW170817 was that, even after it was detected, it sustained a slow brightening at all wavelengths (Margutti et al., 2017; Mooley et al., 2018c; Ruan et al., 2018; Troja et al., 2019b), eventually peaking
The outflow from GW170817 along the direction toward Earth was under-energetic by a factor 10,000 to 100,000 times with respect to a typical SGRB (Fong et al., 2017). An outstanding question was therefore whether GW170817 had a misaligned, SGRB-like jet pointing in a different direction or not (Lazzati et al., 2018; Mooley et al., 2018a; Salafia et al., 2018). If it did, then the identification of the SGRB progenitors with binary NS mergers would be secured. If did not, then what GW10817 was associated with would be a new class of dim, possibly isotropic, γ-ray transients. Unfortunately, telling whether a misaligned relativistic jet is present is not easy, since all the radiation is relativistically beamed away from the line of sight. The slow but steady brightening was shown to be consistent with the presence of a jet, its energy contribution along the line of sight growing with the deceleration of the external shock (Xiao et al., 2017; De Colle et al., 2018; Finstad et al., 2018; Granot et al., 2018b; Lamb and Kobayashi, 2018; Lazzati et al., 2018; Nakar et al., 2018; Fraija et al., 2019a; Fraija et al., 2019b; Beniamini et al., 2020b; Oganesyan et al., 2020). However, a radially stratified spherical outflow could reproduce the observations as well, albeit at the price of adding a never observed before component to the models (Li et al., 2018; Mooley et al., 2018c; Nakar et al., 2018; Nakar and Piran, 2018; Salafia et al., 2018). Some evidence in favor of a jet was provided by the steep post-peak decay at all wavelengths (Alexander et al., 2018; Jin et al., 2018; Lamb et al., 2018; Mooley et al., 2018b; Nynka et al., 2018; Fong et al., 2019; Hajela et al., 2019). In addition, it was soon realized that either a relatively large linear polarization (Gill and Granot, 2018) or a small but detectable proper motion of the radio transient could potentially give the final clue. Both observations were carried out. Polarization turned out to be small (Corsi et al., 2018), and only an upper limit of 12 per cent was obtained, still consistent with either explanation. Long baseline radio interferometry turned out to be the key. In one experiment, a small but significant proper motion was detected (Mooley et al., 2018a), while in a second experiment the radio source was confirmed to be point-like (Ghirlanda et al., 2019). Both these characteristics are incompatible with a spherical expansion. In the future, the detection of the counter-jet emission might give additional evidence (Yamazaki 2018).
To date, despite the very high quality of the available data, the unique afterglow of GW170817 can be modeled successfully with the good old external shock synchrotron model (Mészáros and Rees, 1997; Sari et al., 1998), with the only required addition of considering off-axis observers (Granot et al., 2002) and allowing for some structure in the polar direction (Lazzati et al., 2017b; Lazzati et al., 2018). The type of polar stratification is not univocally constrained, since Gaussian, power-law, and exponential profile seem all to give an adequate fit to the data (Lazzati et al., 2018; Troja et al., 2018a; Xie et al., 2018; Ghirlanda et al., 2019). Numerical simulations are also ambiguous, different codes yielding different polar structures, including the three mentioned above (Murguia-Berthier et al., 2014; Nagakura et al., 2014; Lazzati et al., 2017b; Murguia-Berthier et al., 2017a; Murguia-Berthier et al., 2017b; Duffell et al., 2018; Granot et al., 2018a; Wu and MacFadyen, 2018; Xie et al., 2018; Geng et al., 2019; Gill et al., 2019b; Kathirgamaraju et al., 2019; Hamidani et al., 2020). Constraints can be obtained from the lack of a large populations of cosmological off-axis bursts (Beniamini 2019). More observations and further theoretical work are needed to pin down this important aspect that has implications not only on the detectability of bursts but also on the nature of the inner engine and the composition of the ejected jet and wind.
5 Summary, Discussion, and a Look at the Future
GW170817 was a rich event, a cornerstone detection in our understanding of SGRBs. It confirmed that binary NS mergers are the progenitor of at least some short bursts, it showed us that the top-hat jet model is woefully inadequate for describing the relativistic outflows of SGRBs (and possibly long duration GRBs as well) and it gave us, for the first time ever, a measure of the trigger time and of the delay between the launching of the jet and the detection of the prompt emission radiation.
We now know that the burst associated with GW170817 was a fairly canonical SGRB (Salafia et al., 2019), with a powerful relativistic jet that, after interacting with the merger wind, turned into a structured outflow (Lazzati et al., 2017b; Lazzati et al., 2018). Our line of sight lied somewhere between 15° and 35° away from the jet axis, the lower value obtained by high resolution radio imaging (Mooley et al., 2018c; Ghirlanda et al., 2019), while the larger value being favored by multi-band afterglow modeling and ejecta considerations (Lazzati et al., 2018; Mandel, 2018; Zou et al., 2018). The prompt emission was powered by an energetic cocoon inflated by the interaction of the jet with the merger wind. The gamma-ray radiation was likely released at or near the photosphere, either by a shock breakout (Nakar and Sari, 2012; Kasliwal et al., 2017; Gottlieb et al., 2018) or by other non-thermal mechanisms (Savchenko et al., 2017; Veres et al., 2018). The external shock developed later than usual due to the lower than customary Lorentz factor of the outflow along the line of sight and the afterglow was unusual, characterized by an initial increase in luminosity that lasted for a few months before peaking and beginning a steep declining phase. This behavior is understood to be due to the structure of the outflow, characterized by a polar stratification with a steep decline as a function of angle in both the energy per unit solid angle and the Lorentz factor.
Despite the large amount of observational evidence that allowed us to paint a detailed picture of the dynamic of the relativistic ejecta of GW170817 and their electromagnetic signatures, some questions remain open. First, we do not know the nature of the compact object that launched the relativistic jet. It could have been either a meta-stable NS or a BH, and consensus in this respect hasn’t been reached (Piro et al., 2019; Metzger et al., 2018; Pooley et al., 2018; Abedi and Afshordi, 2019). A related mystery is the origin of the observed 1.75 s delay between the GW and the prompt emission. As discussed in Section 2.1 the delay is the sum of many components and it is unclear which dominates, or if several of them have comparable magnitude. Since the photospheric delay is strongly dependent on the viewing angle, observation of several SGRBs from a diverse set of angles will help better understand the origin of the delay. Still unclear is also the physics of the dissipation that powered the prompt emission and the prompt emission mechanism itself. Shock breakouts, internal dissipation such as internal shocks, and even external shocks have been proposed (see Section 3).
Finally, we still do not know how typical GW170817 was. The fact that most likely it originated from a binary NS merger does not exclude the possibility that some—if not most—SGRB are made in NS-BH mergers. It might even be that GW170817 itself was a NS-BH merger (Coughlin and Dietrich, 2019; Kyutoku et al., 2020). Re-analysis of several past bursts have yielded some support the presence of kilonovae in their light curves (Troja et al., 2018b; Beniamini et al., 2019; Lamb et al., 2019b; Troja et al., 2019a) or similarities in their prompt emission (Burns 2018, von Kienlin 2019), showing that GW170817 was not unique. However, there might be cases in which the jet is not successful in breaking out of the wind leading edge, and a weaker transient would be produced (Kasliwal et al., 2017; Mooley et al., 2018c; Salafia et al., 2018). Future GW detections with the power of multimessenger observations will allow to better understand the connection between binary NS mergers, binary NS-BH mergers, and SGRBs.
DL has written this review article on his own to the best of his knowledge, he has produced all figures himself from publicly available data and codes. The references are extensive but they are by no means exhaustive.
Conflict of Interest
The authors declare that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.
DL acknowledges support from NASA grants 80NSSC18K1729 (Fermi) and NNX17AK42G (ATP), Chandra grant TM9-20002X, and NSF grant AST-1907955.
Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., et al. (2017a). GW170817: Observation of gravitational waves from a binary neutron star inspiral. Phys. Rev. Lett. 119, 161101. doi:10.1103/PhysRevLett.119.161101
Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., et al. (2017b). Gravitational waves and gamma-rays from a binary neutron star merger: GW170817 and GRB 170817A. Astrophys. J. 848, L13. doi:10.3847/2041-8213/aa920c
Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., et al. (2017c). Multi-messenger observations of a binary neutron star merger. Astrophys. J. 848, L12. doi:10.3847/2041-8213/aa91c9
Abdalla, H., Abramowski, A., Aharonian, F., Ait Benkhali, F., Angüner, E. O., Arakawa, M., et al. (2017). TeV gamma-ray observations of the binary neutron star merger GW170817 with H.E.S.S. Astrophys. J. Lett. 850, L22. doi:10.3847/2041-8213/aa97d2
Abedi, J., and Afshordi, N. (2019). Echoes from the abyss: a highly spinning black hole remnant for the binary neutron star merger GW170817. J. Cosmol. Astropart. Phys. 2019, 010. doi:10.1088/1475-7516/2019/11/010
Alexander, K. D., Berger, E., Fong, W., Williams, P. K. G., Guidorzi, C., Margutti, R., et al. (2017). The electromagnetic counterpart of the binary neutron star merger LIGO/virgo GW170817. VI. Radio constraints on a relativistic jet and predictions for late-time emission from the kilonova ejecta. Astrophys. J. 848, L21. doi:10.3847/2041-8213/aa905d
Alexander, K. D., Margutti, R., Blanchard, P. K., Fong, W., Berger, E., Hajela, A., et al. (2018). A decline in the X-ray through radio emission from GW170817 continues to support an off-axis structured jet. Astrophys. J. 863, L18. doi:10.3847/2041-8213/aad637
Aloy, M. A., Janka, H.-T., and Müller, E. (2005). Relativistic outflows from remnants of compact object mergers and their viability for short gamma-ray bursts. Astron. Astrophys. 436, 273–311. doi:10.1051/0004-6361:20041865
Arcavi, I., Hosseinzadeh, G., Howell, D. A., McCully, C., Poznanski, D., Kasen, D., et al. (2017). Optical emission from a kilonova following a gravitational-wave-detected neutron-star merger. Nature 551, 64–66. doi:10.1038/nature24291
Belczynski, K., Perna, R., Bulik, T., Kalogera, V., Ivanova, N., and Lamb, D. Q. (2006). A study of compact object mergers as short gamma‐ray burst progenitors. Astrophys. J. 648, 1110–1116. doi:10.1086/505169
Beniamini, P., Duran, R. B., Petropoulou, M., and Giannios, D. (2020a). Ready, set, launch: time interval between a binary neutron star merger and short gamma-ray burst jet formation. Astrophys. J. 895, L33. doi:10.3847/2041-8213/ab9223
Beniamini, P., Petropoulou, M., Barniol Duran, R., and Giannios, D. (2019). A lesson from GW170817: most neutron star mergers result in tightly collimated successful GRB jets. Mon. Not. R. Astron. Soc. 483, 840–851. doi:10.1093/mnras/sty3093
Bromberg, O., Nakar, E., Piran, T., and Sari, R. E. (2013). Short versus long and collapsars versus non-collapsars: a quantitative classification of gamma-ray bursts. Astrophys. J. 764, 179. doi:10.1088/0004-637X/764/2/179
Bromberg, O., Tchekhovskoy, A., Gottlieb, O., Nakar, E., and Piran, T. (2018). The γ-rays that accompanied GW170817 and the observational signature of a magnetic jet breaking out of NS merger ejecta. Mon. Not. R. Astron. Soc. 475, 2971–2977. doi:10.1093/mnras/stx3316
Bucciantini, N., Quataert, E., Arons, J., Metzger, B. D., and Thompson, T. A. (2008). Relativistic jets and long-duration gamma-ray bursts from the birth of magnetars. Mon. Not. R. Astron. Soc. Lett. 383, L25–L29. doi:10.1111/j.1745-3933.2007.00403.x
Bucciantini, N., Quataert, E., Metzger, B. D., Thompson, T. A., Arons, J., and Del Zanna, L. (2009). Magnetized relativistic jets and long-duration GRBs from magnetar spin-down during core-collapse supernovae. Mon. Not. R. Astron. Soc. 396, 2038–2050. doi:10.1111/j.1365-2966.2009.14940.x
Burns, E., Veres, P., Connaughton, V., Racusin, J., Briggs, M.-S., and Christensen, N. (2018). Fermi GBM observations of GRB 150101B: a second nearby event with a short hard spike and a soft tail. apjl 863 (2), L34. doi:10.3847/2041-8213/aad813.
Corsi, A., Hallinan, G. W., Lazzati, D., Mooley, K. P., Murphy, E. J., Frail, D. A., et al. (2018). An upper limit on the linear polarization fraction of the GW170817 radio continuum. Astrophys. J. 861, L10. doi:10.3847/2041-8213/aacdfd
Coulter, D. A., Foley, R. J., Kilpatrick, C. D., Drout, M. R., Piro, A. L., Shappee, B. J., et al. (2017). Swope Supernova Survey 2017a (SSS17a), the optical counterpart to a gravitational wave source. Science 358, 1556–1558. doi:10.1126/science.aap9811
Cowperthwaite, P. S., Berger, E., Villar, V. A., Metzger, B. D., Nicholl, M., Chornock, R., et al. (2017). The electromagnetic counterpart of the binary neutron star merger LIGO/virgo GW170817. II. UV, optical, and near-infrared light curves and comparison to kilonova models. Astrophys. J. 848, L17. doi:10.3847/2041-8213/aa8fc7
Dainotti, M. G., Hernandez, X., Postnikov, S., Nagataki, S., O’brien, P., Willingale, R., et al. (2017). A study of the gamma-ray burst fundamental plane. Astrophys. J. 848, 88. doi:10.3847/1538-4357/aa8a6b
Dainotti, M. G., Willingale, R., Capozziello, S., Cardone, V. F., and Ostrowski, M . (2010). Discovery of a tight correlation for gamma-ray burst afterglows with “canonical” light curves. Astrophys. J. 722, L215–L219. doi:10.1088/2041-8205/722/2/L215
D’Avanzo, P., Campana, S., Salafia, O. S., Ghirland, A. G., Ghisellini, G., Melandri, A., et al. (2018). The evolution of the X-ray afterglow emission of GW 170817/GRB 170817A in XMM-Newton observations. Astron. Astrophys. 613, L1. doi:10.1051/0004-6361/201832664
De Colle, F., Kumar, P., and Aguilera-Dena, D. R. (2018). Radio emission from the cocoon of a GRB jet: implications for relativistic supernovae and off-axis GRB emission. Astrophys. J. 863, 1. doi:10.3847/1538-4357/aad04d
Evans, P. A., Cenko, S. B., Kennea, J. A., Emery, S. W. K., Kuin, N. P. M., Korobkin, O., et al. (2017). SwiftandNuSTARobservations of GW170817: detection of a blue kilonova. Science 358, 1565–1570. doi:10.1126/science.aap9580
Finstad, D., De, S., Brown, D. A., Berger, E., and Biwer, C. M. (2018). Measuring the viewing angle of GW170817 with electromagnetic and gravitational waves. Astrophys. J. 860, L2. doi:10.3847/2041-8213/aac6c1
Fong, W., Blanchard, P. K., Alexander, K. D., Strader, J., Margutti, R., Hajela, A., et al. (2019). The optical afterglow of GW170817: an off-axis structured jet and deep constraints on a globular cluster origin. Astrophys. J. 883, L1. doi:10.3847/2041-8213/ab3d9e
Fong, W., Berger, E., Blanchard, P. K., Margutti, R., Cowperthwaite, P. S., Chornock, R., et al. (2017). The electromagnetic counterpart of the binary neutron star merger LIGO/virgo GW170817. VIII. A comparison to cosmological short-duration gamma-ray bursts. Astrophys. J. 848, L23. doi:10.3847/2041-8213/aa9018
Fong, W., Berger, E., Margutti, R., and Zauderer, B. A. (2015). A decade of short-duration gamma-ray burst broadband Afterglows: energetics, circumburst densities, and jet opening angles. Astrophys. J. 815, 102. doi:10.1088/0004-637X/815/2/102
Fraija, N., Colle, F. D., Veres, P., Dichiara, S., Duran, R. B., Galvan-Gamez, A., et al. (2019a). The short GRB 170817A: modeling the off-axis emission and implications on the ejecta magnetization. Astrophys. J. 871, 123. doi:10.3847/1538-4357/aaf564
Fraija, N., Pedreira, A. C. C. D. E. S., and Veres, P. (2019b). Light curves of a shock-breakout material and a relativistic off-axis jet from a binary neutron star system. Astrophys. J. 871, 200. doi:10.3847/1538-4357/aaf80e
Geng, J. J., Zhang, B., Kölligan, A., Kuiper, R., and Huang, Y. F. (2019). Propagation of a short GRB jet in the ejecta: jet launching delay time, jet structure, and GW170817/GRB 170817A. Astrophys. J. 877, L40. doi:10.3847/2041-8213/ab224b
Ghirlanda, G., Salafia, O. S., Paragi, Z., Giroletti, M., Yang, J., Marcote, B., et al. (2019). Compact radio emission indicates a structured jet was produced by a binary neutron star merger. Science 363, 968–971. doi:10.1126/science.aau8815
Ghirlanda, G., Salafia, O. S., Pescalli, A., Ghisellini, G., Salvaterra, R., Chassande–Mottin, E., et al. (2016). Short gamma-ray bursts at the dawn of the gravitational wave era. Astron. Astrophys. 594, A84. doi:10.1051/0004-6361/201628993
Gill, R., and Granot, J. (2018). Afterglow imaging and polarization of misaligned structured GRB jets and cocoons: breaking the degeneracy in GRB 170817A. Mon. Not. R. Astron. Soc. 478, 4128–4141. doi:10.1093/mnras/sty1214
Gill, R., Granot, J., De Colle, F., and Urrutia, G. (2019a). Numerical simulations of an initially top-hat jet and the afterglow of GW170817/GRB170817A. Astrophys. J. 883, 15. doi:10.3847/1538-4357/ab3577
Goldstein, A., Veres, P., Burns, E., Briggs, M. S., Hamburg, R., Kocevski, D., et al. (2017). An ordinary short gamma-ray burst with extraordinary implications: Fermi -GBM detection of GRB 170817A. Astrophys. J. 848, L14. doi:10.3847/2041-8213/aa8f41
Gottlieb, O., Nakar, E., Piran, T., and Hotokezaka, K. (2018). A cocoon shock breakout as the origin of the γ-ray emission in GW170817. Mon. Not. R. Astron. Soc. 479, 588–600. doi:10.1093/mnras/sty1462
Granot, J., De Colle, F., and Ramirez-Ruiz, E. (2018a). Off-axis afterglow light curves and images from 2D hydrodynamic simulations of double-sided GRB jets in a stratified external medium. Mon. Not. R. Astron. Soc. 481, 2711–2720. doi:10.1093/mnras/sty2454
Granot, J., Gill, R., Guetta, D., and De Colle, F. (2018b). Off-axis emission of short GRB jets from double neutron star mergers and GRB 170817A. Mon. Not. R. Astron. Soc. 481, 1597–1608. doi:10.1093/mnras/sty2308
Granot, J., Guetta, D., and Gill, R. (2017). Lessons from the short GRB 170817A: the first gravitational-wave detection of a binary neutron star merger. Astrophys. J. 850, L24. doi:10.3847/2041-8213/aa991d
Haggard, D., Nynka, M., Ruan, J. J., Kalogera, V., Cenko, S. B., Evans, P., et al. (2017). A deep Chandra X-ray study of neutron star coalescence GW170817. Astrophys. J. 848, L25. doi:10.3847/2041-8213/aa8ede
Hajela, A., Margutti, R., Alexander, K. D., Kathirgamaraju, A., Baldeschi, A., Guidorzi, C., et al. (2019). Two years of nonthermal emission from the binary neutron star merger GW170817: rapid fading of the jet afterglow and first constraints on the kilonova fastest ejecta. Astrophys. J. 886, L17. doi:10.3847/2041-8213/ab5226
Jin, Z.-P., Li, X., Wang, H., Wang, Y.-Z., He, H.-N., Yuan, Q., et al. (2018). Short GRBs: opening angles, local neutron star merger rate, and off-axis events for GRB/GW association. Astrophys. J. 857, 128. doi:10.3847/1538-4357/aab76d
Kasen, D., Metzger, B., Barnes, J., Quataert, E., and Ramirez-Ruiz, E. (2017). Origin of the heavy elements in binary neutron-star mergers from a gravitational-wave event. Nature 551, 80–84. doi:10.1038/nature24453
Kasliwal, M. M., Nakar, E., Singer, L. P., Kaplan, D. L., Cook, D. O., Van Sistine, A., et al. (2017). Illuminating gravitational waves: a concordant picture of photons from a neutron star merger. Science 358, 1559–1565. doi:10.1126/science.aap9455
Kathirgamaraju, A., Tchekhovskoy, A., Giannios, D., and Barniol Duran, R. (2019). EM counterparts of structured jets from 3D GRMHD simulations. Mon. Not. R. Astron. Soc. 484, L98–L103. doi:10.1093/mnrasl/slz012
Kim, S., Schulze, S., Resmi, L., González-López, J., Higgins, A. B., Ishwara-Chandra, C. H., et al. (2017). ALMA and GMRT constraints on the off-axis gamma-ray burst 170817A from the binary neutron star merger GW170817. Astrophys. J. 850, L21. doi:10.3847/2041-8213/aa970b
Kisaka, S., Ioka, K., Kashiyama, K., and Nakamura, T. (2018). Scattered short gamma-ray bursts as electromagnetic counterparts to gravitational waves and implications of GW170817 and GRB 170817A. Astrophys. J. 867, 39. doi:10.3847/1538-4357/aae30a
Kiuchi, K., Sekiguchi, Y., Shibata, M., and Taniguchi, K. (2010). Exploring binary-neutron-star-merger scenario of short-gamma-ray bursts by gravitational-wave observation. Phys. Rev. Lett. 104, 141101. doi:10.1103/PhysRevLett.104.141101
Kouveliotou, C., Meegan, C. A., Fishman, G. J., Bhat, N. P., Briggs, M. S., Koshut, T. M., et al. (1993). Identification of two classes of gamma-ray bursts. Astrophys. J. 413, L101. doi:10.1086/186969
Kyutoku, K., Fujibayashi, S., Hayashi, K., Kawaguchi, K., Kiuchi, K., Shibata, M., et al. (2020). On the possibility of GW190425 being a black hole-neutron star binary merger. Astrophys. J. 890, L4. doi:10.3847/2041-8213/ab6e70
Lamb, G. P., Lyman, J. D., Levan, A. J., Tanvir, N. R., Kangas, T., Fruchter, A. S., et al. (2019a). The optical afterglow of GW170817 at one year post-merger. Astrophys. J. 870, L15. doi:10.3847/2041-8213/aaf96b
Lamb, G. P., Tanvir, N. R., Levan, A. J., Postigo, A. D. U., Kawaguchi, K., Corsi, A., et al. (2019b). Short GRB 160821B: a reverse shock, a refreshed shock, and a well-sampled kilonova. Astrophys. J. 883, 48. doi:10.3847/1538-4357/ab38bb
Lazzati, D., Ciolfi, R., and Perna, R. (2020). Intrinsic properties of the engine and jet that powered the short gamma-ray burst associated with GW170817. Astrophys. J. 898, 1–59. doi:10.3847/1538-4357/ab9a44
Lazzati, D., Deich, A., Morsony, B. J., and Workman, J. C. (2017a). Off-axis emission of short γ-ray bursts and the detectability of electromagnetic counterparts of gravitational-wave-detected binary mergers. Mon. Not. R. Astron. Soc. 471, 1652–1661. doi:10.1093/mnras/stx1683
Lazzati, D., López-Cámara, D., Cantiello, M., Morsony, B. J., Perna, R., and Workman, J. C. (2017b). Off-axis prompt X-ray transients from the cocoon of short gamma-ray bursts. Astrophys. J. 848, L6. doi:10.3847/2041-8213/aa8f3d
Lazzati, D., Perna, R., Morsony, B. J., Lopez-Camara, D., Cantiello, M., Ciolfi, R., et al. (2018). Late time afterglow observations reveal a collimated relativistic jet in the ejecta of the binary neutron star merger GW170817. Phys. Rev. Lett. 120, 241103. doi:10.1103/PhysRevLett.120.241103
Lei, W.-H., Zhang, B., and Liang, E.-W. (2013). Hyperaccreting black hole as gamma-ray burst central engine. I. Baryon loading in gamma-ray burst jets. Astrophys. J. 765, 125. doi:10.1088/0004-637X/765/2/125
Li, B., Li, L.-B., Huang, Y.-F., Geng, J.-J., Yu, Y.-B., and Song, L.-M. (2018). Continued brightening of the afterglow of GW170817/GRB 170817A as being due to a delayed energy injection. Astrophys. J. 859, L3. doi:10.3847/2041-8213/aac2c5
Lin, D.-B., Liu, T., Lin, J., Wang, X.-G., Gu, W.-M., and Liang, E.-W. (2018). First electromagnetic pulse associated with a gravitational-wave event: profile, duration, and delay. Astrophys. J. 856, 90. doi:10.3847/1538-4357/aab3d7
Liu, T., Romero, G. E., Liu, M.-L., and Li, A. (2016). Fast radio bursts and their gamma-ray or radio afterglows as kerr-newman black hole binaries. . apj 826 (1), 82.. doi:10.3847/0004-637X/826/1/82.
Lyman, J. D., Lamb, G. P., Levan, A. J., Mandel, I., Tanvir, N. R., Kobayashi, S., et al. (2018). The optical afterglow of the short gamma-ray burst associated with GW170817. Nat. Astron. 2, 751–754. doi:10.1038/s41550-018-0511-3
Makhathini, S., Mooley, K. P., Brightman, M., Hotokezaka, K., Nayana, A., Intema, H. T., et al. (2020). The Panchromatic Afterglow of GW170817: the full uniform dataset, modeling, comparison with previous results and implications. arXiv e-prints arXiv:2006.02382.
Margutti, R., Alexander, K. D., Xie, X., Sironi, L., Metzger, B. D., Kathirgamaraju, A., et al. (2018). The binary neutron star event LIGO/virgo GW170817 160 Days after merger: synchrotron emission across the electromagnetic spectrum. Astrophys. J. 856, L18. doi:10.3847/2041-8213/aab2ad
Margutti, R., Berger, E., Fong, W., Guidorzi, C., Alexander, K. D., Metzger, B. D., et al. (2017). The electromagnetic counterpart of the binary neutron star merger LIGO/virgo GW170817. V. Rising X-ray emission from an off-axis jet. Astrophys. J. 848, L20. doi:10.3847/2041-8213/aa9057
Meng, Y.-Z., Geng, J.-J., Zhang, B.-B., Wei, J.-J., Xiao, D., Liu, L.-D., et al. (2018). The origin of the prompt emission for short GRB 170817A: photosphere emission or synchrotron emission? Astrophys. J. 860, 72. doi:10.3847/1538-4357/aac2d9
Metzger, B. D., Giannios, D., Thompson, T. A., Bucciantini, N., and Quataert, E. (2011). The protomagnetar model for gamma-ray bursts. Mon. Not. R. Astron. Soc. 413, 2031–2056. doi:10.1111/j.1365-2966.2011.18280.x
Mooley, K. P., Deller, A. T., Gottlieb, O., Nakar, E., Hallinan, G., Bourke, S., et al. (2018a). Superluminal motion of a relativistic jet in the neutron-star merger GW170817. Nature 561, 355–359. doi:10.1038/s41586-018-0486-3
Mooley, K. P., Frail, D. A., Dobie, D., Lenc, E., Corsi, A., De, K., et al. (2018b). A strong jet signature in the late-time light curve of GW170817. Astrophys. J. 868, L11. doi:10.3847/2041-8213/aaeda7
Mooley, K. P., Nakar, E., Hotokezaka, K., Hallinan, G., Corsi, A., Frail, D. A., et al. (2018c). A mildly relativistic wide-angle outflow in the neutron-star merger event GW170817. Nature 554, 207–210. doi:10.1038/nature25452
Murguia-Berthier, A., Montes, G., Ramirez-Ruiz, E., De Colle, F., and Lee, W. H. (2014). Necessary conditions for short gamma-ray burst production in binary neutron star mergers. Astrophys. J. 788, L8. doi:10.1088/2041-8205/788/1/L8
Murguia-Berthier, A., Ramirez-Ruiz, E., Kilpatrick, C. D., Foley, R. J., Kasen, D., Lee, W. H., et al. (2017a). A neutron star binary merger model for GW170817/GRB 170817A/SSS17a. Astrophys. J. 848, L34. doi:10.3847/2041-8213/aa91b3
Murguia-Berthier, A., Ramirez-Ruiz, E., Montes, G., De Colle, F., Rezzolla, L., Rosswog, S., et al. (2017b). The properties of short gamma-ray burst jets triggered by neutron star mergers. Astrophys. J. 835, L34. doi:10.3847/2041-8213/aa5b9e
Nagakura, H., Hotokezaka, K., Sekiguchi, Y., Shibata, M., and Ioka, K. (2014). Jet collimation in the ejecta of double neutron star mergers: a new canonical picture of short gamma-ray bursts. Astrophys. J. 784, L28. doi:10.1088/2041-8205/784/2/L28
Nakar, E., Gal‐Yam, A., and Fox, D. B. (2006). The local rate and the progenitor lifetimes of short‐hard gamma‐ray bursts: synthesis and predictions for the laser interferometer gravitational‐wave observatory. Astrophys. J. 650, 281–290. doi:10.1086/505855
Nakar, E., and Sari, R. E. (2012). Relativistic shock breakouts-a variety of gamma-ray flares: from low-luminosity gamma-ray bursts to type ia supernovae. Astrophys. J. 747, 88. doi:10.1088/0004-637X/747/2/88
Nousek, J. A., Kouveliotou, C., Grupe, D., Page, K. L., Granot, J., Ramirez‐Ruiz, E., et al. (2006). Evidence for a canonical gamma‐ray burst afterglow light curve in theSwiftXRT data. Astrophys. J. 642, 389–400. doi:10.1086/500724
Nynka, M., Ruan, J. J., Haggard, D., and Evans, P. A. (2018). Fading of the X-ray afterglow of neutron star merger GW170817/GRB 170817A at 260 days. Astrophys. J. 862, L19. doi:10.3847/2041-8213/aad32d
Oganesyan, G., Ascenzi, S., Branchesi, M., Salafia, O. S., Dall’Osso, S., and Ghirlanda, G. (2020). Structured jets and X-ray plateaus in gamma-ray burst phenomena. Astrophys. J. 893, 88. doi:10.3847/1538-4357/ab8221
Pian, E., D’Avanzo, P., Benetti, S., Branchesi, M., Brocato, E., Campana, S., et al. (2017). Spectroscopic identification of r-process nucleosynthesis in a double neutron-star merger. Nature 551, 67–70. doi:10.1038/nature24298
Piro, L., Troja, E., Zhang, B., Ryan, G., van Eerten, H., Ricci, R., et al. (2019). A long-lived neutron star merger remnant in GW170817: constraints and clues from X-ray observations. Mon. Not. R. Astron. Soc. 483, 1912–1921. doi:10.1093/mnras/sty3047
Pozanenko, A. S., Barkov, M. V., Minaev, P. Y., Volnova, A. A., Mazaeva, E. D., Moskvitin, A. S., et al. (2018). GRB 170817A associated with GW170817: multi-frequency observations and modeling of prompt gamma-ray emission. Astrophys. J. 852, L30. doi:10.3847/2041-8213/aaa2f6
Ramirez-Ruiz, E., Celotti, A., and Rees, M. J. (2002). Events in the life of a cocoon surrounding a light, collapsar jet. Mon. Not. R. Astron. Soc. 337, 1349–1356. doi:10.1046/j.1365-8711.2002.05995.x
Resmi, L., Schulze, S., Ishwara-Chandra, C. H., Misra, K., Buchner, J., Pasquale, M. D., et al. (2018). Low-frequency view of GW170817/GRB 170817A with the giant metrewave radio telescope. Astrophys. J. 867, 57. doi:10.3847/1538-4357/aae1a6
Ruan, J. J., Nynka, M., Haggard, D., Kalogera, V., and Evans, P. (2018). Brightening X-ray emission from GW170817/GRB 170817A: further evidence for an outflow. Astrophys. J. 853, L4. doi:10.3847/2041-8213/aaa4f3
Salafia, O. S., Barbieri, C., Ascenzi, S., and Toffano, M. (2020). Gamma-ray burst jet propagation, development of angular structure, and the luminosity function. Astron. Astrophys. 636, A105. doi:10.1051/0004-6361/201936335
Salafia, O. S., Ghisellini, G., Ghirlanda, G., and Colpi, M. (2018). Interpreting GRB170817A as a giant flare from a jet-less double neutron star merger. Astron. Astrophys. 619, A18. doi:10.1051/0004-6361/201732259
Savchenko, V., Ferrigno, C., Kuulkers, E., Bazzano, A., Bozzo, E., Brandt, S., et al. (2017). INTEGRAL detection of the first prompt gamma-ray signal coincident with the gravitational-wave event GW170817. Astrophys. J. 848, L15. doi:10.3847/2041-8213/aa8f94
Shoemaker, I. M., and Murase, K. (2018). Constraints from the time lag between gravitational waves and gamma rays: implications of GW170817 and GRB 170817A. Phys. Rev. D 97, 083013. doi:10.1103/PhysRevD.97.083013
Siebert, M. R., Foley, R. J., Drout, M. R., Kilpatrick, C. D., Shappee, B. J., Coulter, D. A., et al. (2017). The unprecedented properties of the first electromagnetic counterpart to a gravitational-wave source. Astrophys. J. 848, L26. doi:10.3847/2041-8213/aa905e
Smartt, S. J., Chen, T. W., Jerkstrand, A., Coughlin, M., Kankare, E., Sim, S. A., et al. (2017). A kilonova as the electromagnetic counterpart to a gravitational-wave source. Nature 551, 75–79. doi:10.1038/nature24303
Soares-Santos, M., Holz, D. E., Annis, J., Chornock, R., Herner, K., Berger, E., et al. (2017). The electromagnetic counterpart of the binary neutron star merger LIGO/virgo GW170817. I. Discovery of the optical counterpart using the dark energy camera. Astrophys. J. 848, L16. doi:10.3847/2041-8213/aa9059
Tanvir, N. R., Levan, A. J., González-Fernández, C., Korobkin, O., Mandel, I., Rosswog, S., et al. (2017). The emergence of a lanthanide-rich kilonova following the merger of two neutron stars. Astrophys. J. 848, L27. doi:10.3847/2041-8213/aa90b6
Troja, E., Castro-Tirado, A. J., González, J. B., Hu, Y., Ryan, G. S., Cenko, S. B., et al. (2019a). The afterglow and kilonova of the short GRB 160821B. Mon. Not. R. Astron. Soc. 489, 2104–2116. doi:10.1093/mnras/stz2255
Troja, E., Piro, L., Ryan, G., van Eerten, H., Ricci, R., Wieringa, M. H., et al. (2018a). The outflow structure of GW170817 from late-time broad-band observations. Mon. Not. R. Astron. Soc. 478, L18–L23. doi:10.1093/mnrasl/sly061
Troja, E., Ryan, G., Piro, L., van Eerten, H., Cenko, S. B., Yoon, Y., et al. (2018b). A luminous blue kilonova and an off-axis jet from a compact binary merger at z = 0.1341. Nat. Commun. 9, 4089. doi:10.1038/s41467-018-06558-7
Troja, E., van Eerten, H., Ryan, G., Ricci, R., Burgess, J. M., Wieringa, M. H., et al. (2019b). A year in the life of GW170817: the rise and fall of a structured jet from a binary neutron star merger. Mon. Not. R. Astron. Soc. 489, 1919–1926. doi:10.1093/mnras/stz2248
Valenti, S., Sand, D. J., Yang, S., Cappellaro, E., Tartaglia, L., Corsi, A., et al. (2017). The discovery of the electromagnetic counterpart of GW170817: kilonova at 2017gfo/DLT17ck. Astrophys. J. 848, L24. doi:10.3847/2041-8213/aa8edf
Veres, P., Mészáros, P., Goldstein, A., Fraija, N., Connaughton, V., Burns, E., et al. (2018). Gamma-ray burst models in light of the GRB 170817A - GW170817 connection. arXiv e-prints arXiv:1802.07328.
Villar, V. A., Cowperthwaite, P. S., Berger, E., Blanchard, P. K., Gomez, S., Alexander, K. D., et al. (2018). Spitzer Space telescope infrared observations of the binary neutron star merger GW170817. Astrophys. J. 862, L11. doi:10.3847/2041-8213/aad281
Wu, Y., and MacFadyen, A. (2018). Constraining the outflow structure of the binary neutron star merger event GW170817/GRB170817A with a Markov chain Monte Carlo analysis. Astrophys. J. 869, 55. doi:10.3847/1538-4357/aae9de
Xiao, D., Liu, L.-D., Dai, Z.-G., and Wu, X.-F. (2017). Afterglows and kilonovae associated with nearby low-luminosity short-duration gamma-ray bursts: application to GW170817/GRB 170817A. Astrophys. J. 850, L41. doi:10.3847/2041-8213/aa9b2b
Xie, X., Zrake, J., and MacFadyen, A. (2018). Numerical simulations of the jet dynamics and synchrotron radiation of binary neutron star merger event GW170817/GRB 170817A. Astrophys. J. 863, 58. doi:10.3847/1538-4357/aacf9c
Zhang, B.-B., Zhang, B., Sun, H., Lei, W.-H., Gao, H., Li, Y., et al. (2018). A peculiar low-luminosity short gamma-ray burst from a double neutron star merger progenitor. Nat. Commun. 9, 447. doi:10.1038/s41467-018-02847-3
Keywords: gamma-ray bursts, relativistic astrophysics, hydrodynamics, gravitational waves, binary mergers, transient sources
Citation: Lazzati D (2020) Short Duration Gamma-Ray Bursts and Their Outflows in Light of GW170817. Front. Astron. Space Sci. 7:578849. doi: 10.3389/fspas.2020.578849
Received: 01 July 2020; Accepted: 11 September 2020;
Published: 09 November 2020.
Edited by:Bruno Giacomazzo, University of Milano-Bicocca, Italy
Reviewed by:Maria Dainotti, Jagiellonian University, Poland
Herman J. Mosquera Cuesta, Departamento Administrativo Nacional de Ciencia, Tecnologia e Innovacion, Colciencias, Colombia
Copyright © 2020 Lazzati. This is an open-access article distributed under the terms of the Creative Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.
*Correspondence: Davide Lazzati, email@example.com