Zobrazeno 1 - 10
of 40
pro vyhledávání: '"Batta, Aldo"'
Autor:
Hutchinson-Smith, Tenley, Everson, Rosa Wallace, Batta, Aldo, Yarza, Ricardo, Twum, Angela A., Law-Smith, Jamie A. P., Ramirez-Ruiz, Enrico
We present a start-to-end simulation aimed at studying the long-term fate of high mass X-ray binaries and whether a Thorne-\.Zytkow object (T\.ZO) might ultimately be produced. We analyze results from a 3D hydrodynamical simulation that models the ev
Externí odkaz:
http://arxiv.org/abs/2311.06741
High-mass X-ray binaries (HMXRBs), such as Cygnus X-1, host some of the most rapidly spinning black holes (BHs) known to date, reaching spin parameters a greater than or similar to 0.84. However, there are several effects that can severely limit the
Externí odkaz:
http://hdl.handle.net/10150/625738
http://arizona.openrepository.com/arizona/handle/10150/625738
http://arizona.openrepository.com/arizona/handle/10150/625738
Autor:
Olivier, Grace M., Lopez, Laura A., Auchettl, Katie, Rosen, Anna L., Batta, Aldo, Neugent, Kathryn F., Ramirez-Ruiz, Enrico, Jayasinghe, Tharindu, Vallely, Patrick J., Rowan, Dominick M.
WR 20a is the most massive close-in binary known in our Galaxy. It is composed of two $\approx$80 M$_\odot$ Wolf-Rayet stars with a short period of $\approx$3.7 days in the open cluster Westerlund 2. As such, WR 20a presents us with a unique laborato
Externí odkaz:
http://arxiv.org/abs/2212.02514
Autor:
Vigna-Gómez, Alejandro, Schrøder, Sophie L., Ramirez-Ruiz, Enrico, Aguilera-Dena, David R., Batta, Aldo, Langer, Norbert, Willcox, Reinhold
The detection of the unusually heavy binary neutron star merger GW190425 marked a stark contrast to the mass distribution from known Galactic pulsars in double neutron star binaries and gravitational-wave source GW170817. We suggest here a formation
Externí odkaz:
http://arxiv.org/abs/2106.12381
Autor:
Murguia-Berthier, Ariadna, Batta, Aldo, Janiuk, Agnieszka, Ramirez-Ruiz, Enrico, Mandel, Ilya, Noble, Scott C., Everson, Rosa Wallace
The collapse of a massive star with low angular momentum content is commonly argued to result in the formation of a black hole without an accompanying bright transient. Our goal in this Letter is to understand the flow in and around a newly-formed bl
Externí odkaz:
http://arxiv.org/abs/2005.10212
Autor:
Bavera, Simone S., Fragos, Tassos, Qin, Ying, Zapartas, Emmanouil, Neijssel, Coenraad J., Mandel, Ilya, Batta, Aldo, Gaebel, Sebastian M., Kimball, Chase, Stevenson, Simon
Publikováno v:
A&A 635, A97 (2020)
We study the formation of coalescing binary black holes via the evolution of isolated field binaries that go through the common envelope phase in order to obtain the combined distributions of the main observables of Advanced LIGO. We used a hybrid te
Externí odkaz:
http://arxiv.org/abs/1906.12257
Autor:
Batta, Aldo, Ramirez-Ruiz, Enrico
Most common formation channels of stellar mass black hole (BH) binaries like the ones observed by LIGO, often assume they are assembled from the direct collapse of massive pre-supernova stars. However, it is still unclear whether the final mass and s
Externí odkaz:
http://arxiv.org/abs/1904.04835
Autor:
Samsing, Johan, Venumadhav, Tejaswi, Dai, Liang, Martinez, Irvin, Batta, Aldo, Lopez Jr., Martin, Ramirez-Ruiz, Enrico, Kremer, Kyle
Publikováno v:
Phys. Rev. D 100, 043009 (2019)
The dynamical assembly of binary black holes (BBHs) in dense star clusters (SCs) is one of the most promising pathways for producing observable gravitational wave (GW) sources, however several other formation scenarios likely operate as well. One of
Externí odkaz:
http://arxiv.org/abs/1901.02889
Binary black holes (BBHs) appear to be widespread and are able to merge through the emission of gravitational waves, as recently illustrated by LIGO. The spin of the BBHs is one of the parameters that LIGO can infer from the gravitational wave signal
Externí odkaz:
http://arxiv.org/abs/1812.01118
Here we investigate within the context of field binary progenitors how the the spin of LIGO sources vary when the helium star-descendent black hole (BH) is formed in a failed supernova (SN) explosion rather than by direct collapse. To this end, we ma
Externí odkaz:
http://arxiv.org/abs/1805.01269