Inhomogeneous Jets from Neutron Star Mergers: One Jet to Rule them all

Lamb, Gavin P.; Nativi, Lorenzo; Rosswog, Stephan; Канн, Д. А.; Levan, A. J.; Tanvir, N. R.

doi:10.48550/arxiv.2201.09796

Cited by 3 publications

(3 citation statements)

References 51 publications

(87 reference statements)

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“…The understanding of the jet-ejecta interaction has been considerably improved, thanks to a wide range of numerical studies in the past years (Kasliwal et al 2017;Lazzati et al 2017;Gottlieb et al 2018aGottlieb et al , 2018bDuffell et al 2018;Kathirgamaraju et al 2018;Geng et al 2019;Lazzati & Perna 2019;Gottlieb et al 2020a;Gottlieb & Loeb 2020;Klion et al 2021;Murguia-Berthier et al 2021;Pavan et al 2021;Urrutia et al 2021;Lamb et al 2022;Nativi et al 2022). However, these studies have been subject to two major limitations:…”

Section: Introductionmentioning

confidence: 99%

On the Jet–Ejecta Interaction in 3D GRMHD Simulations of a Binary Neutron Star Merger Aftermath

Gottlieb¹,

Moseley²,

Ramirez-Aguilar³

et al. 2022

ApJL

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Short γ-ray burst (sGRB) jets form in the aftermath of a neutron star merger, drill through disk winds and dynamical ejecta, and extend over four to five orders of magnitude in distance before breaking out of the ejecta. We present the first 3D general-relativistic magnetohydrodynamic sGRB simulations to span this enormous scale separation. They feature three possible outcomes: jet+cocoon, cocoon, and neither. Typical sGRB jets break out of the dynamical ejecta if (i) the bound ejecta’s isotropic equivalent mass along the pole at the time of the BH formation is ≲10−4 M ⊙, setting a limit on the delay time between the merger and BH formation, otherwise, the jets perish inside the ejecta and leave the jet-inflated cocoon to power a low-luminosity sGRB; (ii) the postmerger remnant disk contains a strong large-scale vertical magnetic field, ≳1015 G; and (iii) if the jets are weak (≲1050 erg), the ejecta’s isotropic equivalent mass along the pole must be small (≲10−2 M ⊙). Generally, the jet structure is shaped by the early interaction with disk winds rather than the dynamical ejecta. As long as our jets break out of the ejecta, they retain a significant magnetization (≲1), suggesting that magnetic reconnection is a fundamental property of sGRB emission. The angular structure of the outflow isotropic equivalent energy after breakout consistently features a flat core followed by a steep power-law distribution (slope ≳3), similar to hydrodynamic jets. In the cocoon-only outcome, the dynamical ejecta broadens the outflow angular distribution and flattens it (slope ∼1.5).

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Section: Introductionmentioning

confidence: 99%

On the Jet–Ejecta Interaction in 3D GRMHD Simulations of a Binary Neutron Star Merger Aftermath

Gottlieb¹,

Moseley²,

Ramirez-Aguilar³

et al. 2022

ApJL

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“…is the on-axis equivalent isotropic energy, E j is the one-side jet energy, and θ c is the characteristic core angle. We adopt a narrow jet structure, where we set θ c ∼ 3°based on recent simulations (e.g., Lamb et al 2022) and observations inferred from the sGRB population (e.g., Jin et al 2018;Lamb et al 2019b). Furthermore, the spectra of the standard synchrotron emission from relativistic electrons are employed following Sari et al (1998), Kumar & Zhang (2015), and Zhang (2018).…”

Section: Optical Afterglow Emissionmentioning

confidence: 99%

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. I. Luminosity Function and Color Evolution

Zhu

Yang

Zhang

et al. 2022

ApJ

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In the first work of this series, we adopt a GW170817-like viewing-angle-dependent kilonova model and the standard afterglow model with a light-curve distribution based on the properties of cosmological short gamma-ray burst afterglows to simulate the luminosity functions and color evolution of both kilonovae and optical afterglow emissions from binary neutron star (BNS) mergers. We find that ∼10% of the nearly-on-axis afterglows are brighter than the associated kilonovae at the peak time. These kilonovae would be significantly polluted by the associated afterglow emission. Only at large viewing angles with sin θ v ≳ 0.20 , the electromagnetic signals of most BNS mergers would be kilonova-dominated and some off-axis afterglows may emerge at ∼5–10 days after the mergers. At a brightness dimmer than ∼23–24 mag, according to their luminosity functions, the number of afterglows is much larger than that of kilonovae. Because the search depth of the present survey projects is <22 mag, the number of afterglow events that are detected via serendipitous observations would be much higher than that of kilonova events, consistent with the current observations. For the foreseeable survey projects (e.g., Mephisto, WFST, and LSST), whose search depths can reach ≳23–24 mag, the detection rate of kilonovae could have the same order of magnitude as afterglows. We also find that it may be difficult to use the fading rate in a single band to directly identify kilonovae and afterglows among various fast-evolving transients by serendipitous surveys. However, the color evolution between the optical and infrared bands can identify them because the color evolution patterns of these phenomena are unique compared with those of other fast-evolving transients.

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“…The understanding of the jet-ejecta interaction has been considerably improved thanks to a wide range of numerical studies in the past years (Kasliwal et al 2017;Lazzati et al 2017;Duffell et al 2018;Gottlieb et al 2018aGottlieb et al ,b, 2020aKathirgamaraju et al 2018;Geng et al 2019;Lazzati & Perna 2019;Gottlieb & Loeb 2020;Klion et al 2021;Murguia-Berthier et al 2021;Pavan et al 2021;Urrutia et al 2021;Nativi et al 2022;Lamb et al 2022). However, these studies have been subject to two major limitations:…”

Section: Introductionmentioning

confidence: 99%

On the jet-ejecta interaction in 3D GRMHD simulations of binary neutron star merger aftermath

Gottlieb,

Moseley,

Ramirez-Aguilar

et al. 2022

Preprint

View full text Add to dashboard Cite

Short γ-ray burst (sGRB) jets form in the aftermath of a neutron star merger, drill through disk winds and dynamical ejecta, and extend over 4-5 orders of magnitude in distance before breaking out of the ejecta. We present the first 3D general-relativistic magnetohydrodynamic sGRB simulations to span this enormous scale separation. They feature three possible outcomes: jet+cocoon, cocoon, and neither. Typical sGRB jets break out of the dynamical ejecta if: (i) the bound ejecta isotropic equivalent mass along the pole at the time of the BH formation is 10 −4 M , setting a limit on the delay time between the merger and BH formation, otherwise the jets perish inside the ejecta and leave the jet-inflated cocoon to power a low-luminosity sGRB; and (ii) postmerger remnant disk contains strong large-scale vertical magnetic field, 10 15 G; and (iii) if the jets are weak ( 10 50 erg), the ejecta isotropic equivalent mass along the pole must be small ( 10 −2 M ). Generally, the jet structure is shaped by the early interaction with disk winds rather than the dynamical ejecta. As long as our jets break out of the ejecta, they retain a significant magnetization ( 1), suggesting that magnetic reconnection is a fundamental property of sGRB emission. The angular structure of the outflow isotropic equivalent energy after breakout consistently features a flat core followed by a steep power-law distribution (slope 3), similar to hydrodynamic jets. In the cocoon-only outcome, the dynamical ejecta broadens the outflow angular distribution and flattens it (slope ∼ 1.5).

show abstract

Inhomogeneous Jets from Neutron Star Mergers: One Jet to Rule them all

Cited by 3 publications

References 51 publications

On the Jet–Ejecta Interaction in 3D GRMHD Simulations of a Binary Neutron Star Merger Aftermath

On the Jet–Ejecta Interaction in 3D GRMHD Simulations of a Binary Neutron Star Merger Aftermath

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. I. Luminosity Function and Color Evolution

On the jet-ejecta interaction in 3D GRMHD simulations of binary neutron star merger aftermath

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