![]() ![]() The NIR magnitudes of the latter are considered as the best “standard candles” and, in this guise, are crucial in modern cosmological studies. WD binary mergers are among the primary candidate mechanisms for type Ia supernovae (SNe Ia) explosions. Its first step should be the launch of ESA’s LISA Pathfinder (LPF) mission in 2015 the launch of eLISA itself is currently planned for 2034. At the moment, eLISA is selected for the third large-class mission in ESA’s Cosmic Vision science program (元). WD binaries, especially those observed as AM CVn-stars and ultracompact X-ray binaries (UCXB), are potential GW sources within the frequency band (10 −4 − 1) Hz of the space GW interferometers like (the currently cancelled) LISA, Footnote 1 NGO (eLISA), DEGIGO and other proposed or planned low-frequency GW detectors. As well, relativistic jets, associated with GRB of any nature may be sources of GW in the ground-based detectors range. A lot of observational support for NS-NS/NS-BH mergers as sources of short GRBs have been obtained (see, e.g., studies of short GRB locations in the host galaxies and references therein). Mergers of NS(BH) binaries can be accompanied by the release of a huge amount of electromagnetic energy in a burst and manifest themselves as short gamma-ray bursts (GRBs). The NS(BH) binary mergers that release ∼ 10 52 erg as GWs should be the brightest GW events in the 10 − 1000 Hz frequency band of the existing or future ground-based GW detectors like LIGO, VIRGO, GEO600, KAGRA(LCGT) (see also for a review of the current state of existing and 2nd- and 3rd-generation ground-based detectors). Close compact binaries can thus serve as testbeds for theories of gravity. ![]() Emission of gravitational waves accompanies the latest stages of evolution of stars and manifests instabilities in relativistic objects. We also consider AM CVn-stars, which are thought to be the best verification binary GW sources for future low-frequency GW space interferometers.Ĭlose binaries consisting of two compact stellar remnants - white dwarfs (WDs), neutron stars (NSs) or black holes (BHs) are considered primary targets of the forthcoming field of gravitational wave (GW) astronomy (see, for a review, ), since their orbital evolution is entirely controlled by the emission of gravitational waves and leads to ultimate coalescence (merger) and possible explosive disruption of the components. ![]() The second part of the review is devoted mainly to the formation and evolution of binary WDs and their observational manifestations, including their role as progenitors of cosmologically-important thermonuclear SN Ia. In the first part of the review, we discuss observational manifestations of close binaries with NS and/or BH components and their merger rate, crucial points in the formation and evolution of compact stars in binary systems, including the treatment of the natal kicks, which NSs and BHs acquire during the core collapse of massive stars and the common envelope phase of binary evolution, which are most relevant to the merging rates of NS-NS, NS-BH and BH-BH binaries. Mergings of compact-star binaries are expected to be the most important sources for forthcoming gravitational-wave (GW) astronomy. We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). ![]()
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |