GW190814: Gravitational Waves from the Coalescence of a 23 Solar Mass Black Hole with a 2.6 Solar Mass Compact Object

Abstract

Gamma-ray bursts (GRBs), associated with the collapse of massive stars or the collisions of compact objects, are the most luminous events in our universe. However, there is still much to learn about the nature of the relativistic jets launched from the central engines of these objects. We examine how jet structure-that is, the energy and velocity distribution as a function of angle-affects observed GRB afterglow light curves. Using the package afterglowpy, we compute light curves arising from an array of possible jet structures, and present the suite of models that can fit the coincident electromagnetic observations of GW190814 (which is likely due to a background AGN). Our work emphasizes not only the need for broadband spectral and timing data to distinguish among jet structure models, but also the necessity for high resolution radio follow-up to help resolve background sources that may mimic a GRB afterglow.

The νR-philic scalar: its loop-induced interactions and Yukawa forces in LIGO observations

“…The muonic long-range force can be tested in binary systems of neutron stars (NS) which contain O(0.1 ∼ 1%) muons of the total mass [55]. In particular, the recent gravitational wave observation of NS binary mergers by the LIGO collaboration [12,13] are able to test the muonic force with unprecedented sensitivity. As indicated by eq.…”

“…For long-range forces mediated by ultralight bosons coupled to electrons or quarks, experimental tests of the strong (based on the lunar laser-ranging technology [9]) and weak (e.g., torsion-balance experiments [10,11]) equivalence principles are sensitive to Yukawa/gauge couplings spanning from 10 −20 to 10 −24 . Very recently, gravitational waves from black hole (BH) and neutron star (NS) binary mergers have been detected by the LIGO/VIRGO collaboration [12,13], providing novel methods to test theories of gravity as well as other long-range forces [14][15][16][17][18][19][20][21][22][23][24]. For instance, the process of BH superradiance can be used to exclude a wide range of ultra-light boson masses [15].…”

Sensitivity and performance of the Advanced LIGO detectors in the third observing run

“…The third observing run (O3), which ran from April 1 to September 30, 2019 (O3a) and from November 1, 2019 until March 27, 2020 (O3b), has been the most successful search for gravitational waves in history, with greater sensitivity and the permanent addition of the Advanced Virgo detector [13]. During this run, 56 candidate gravitational-wave signals, including at least one new compact binary coalescence in the binary neutron star mass range [14] and a system with record mass ratio [15], were announced [16]. The increase in the detection rate is due to the improved performance of the detectors, which is the subject of this paper.…”

Aspectos de relatividade numérica: campos escalares e estrelas de nêutrons

“…However, the difference between two Christoffel symbols is, in fact, a tensor. 11 This means that instead of considering the Christoffel symbolΓ i jk to construct a new auxiliary variable, we can introduce the quantity…”

“…Virgo Scientific Collaboration have detected gravitational waves which have been emitted from different black hole mergers [1][2][3][4][5][6][7] and neutron star binary inspirals [8][9][10]. More recently still, an event has been detected that involves a 23 solar mass black hole and a 2.6 solar mass compact object [11], and our theoretical understanding of this event does not tell us conclusively whether the compact object is the least massive black hole or the most massive neutron star ever detected.…”