J. Dewi
University of Cambridge
6 Papers
11 Citations
J. Dewi is an academic researcher from University of Cambridge. The author has contributed to research in topics: X-ray binary & X-ray burster. The author has an hindex of 4, co-authored 6 publications. Previous affiliations of J. Dewi include Bandung Institute of Technology & University of Amsterdam.
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Papers
The origin and fate of short-period low-mass black-hole binaries
L. R. Yungelson,Jean-Pierre Lasota,Gijs Nelemans,Gijs Nelemans,Guillaume Dubus,Guillaume Dubus,E.P.J. van den Heuvel,J. Dewi,S. Portegies Zwart +8 more
TL;DR: In this article, a population synthesis study for semidetached short orbital period binaries with low-mass (4 M� ) compact accretors is presented, which in their model represent black holes.
The origin and fate of short-period low-mass black-hole binaries
L. R. Yungelson,Jean-Pierre Lasota,Gijs Nelemans,Gijs Nelemans,Guillaume Dubus,Guillaume Dubus,E.P.J. van den Heuvel,J. Dewi,S. Portegies Zwart +8 more
TL;DR: In this article, a population synthesis study for semidetached short orbital period binaries with low-mass (4 Msun) accretors is presented, where the evolution of these binaries is determined by nuclear evolution of the donors and/or orbital angular momentum loss due to magnetic braking by the stellar wind of the donor and gravitational wave radiation.
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CXOU J121538.2+361921 in the galaxy NGC 4214: a double neutron star in the making?
TL;DR: In this paper, it was shown that the X-ray luminosity of CXOU J121538.2+361921 is consistent with super-Eddington accretion in a helium star-neutron star binary.
The ultraluminous X‐ray source in M82: an intermediate‐mass black hole with a giant companion
TL;DR: In this paper, the authors perform detailed binary evolution simulations with an accreting compact object of 10−5000 m and find that the X-ray luminosity, the age of the cluster, the observed quasi-periodic oscillations and the now observed orbital period are explained best by a black hole of 200−5000m⊙ that accretes material from a 22−25 m ⊙ giant companion in a state of Roche-lobe contact.
The formation of the double neutron star pulsar J0737--3039
TL;DR: In this paper, it was shown that the orbital period (2.4 hours), eccentricity (0.09), dipole magnetic field strength (6.9 x 10^9 Gauss) and spin period (22 ms) of the double neutron star system PSR J0737-3039 can all be consistently explained if this system originated from a close helium star plus neutron star binary (HeS-NS) in which at the onset of the evolution the helium star had a mass in the range 4.0 to 6.5 M_sun and an orbital period