Double white dwarfs and
                    <i>LISA</i>

Marsh, T. R.

doi:10.1088/0264-9381/28/9/094019

Cited by 79 publications

(58 citation statements)

References 69 publications

(95 reference statements)

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“…(See [7,8] for deeper reviews.) The most numerous sources in the low-frequency GW sky observed by eLISA will be short-period binaries of two compact objects such as white dwarfs (WDs) or neutron stars (NSs).…”

Section: Compact Binaries In the Galaxymentioning

confidence: 99%

Low-frequency gravitational-wave science with eLISA/NGO

Amaro-Seoane¹,

Aoudia²,

Babak³

et al. 2012

Class. Quantum Grav.

518

567

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We review the expected science performance of the New Gravitational-Wave Observatory (NGO, a.k.a. eLISA), a mission under study by the European Space Agency for launch in the early 2020s. eLISA will survey the low-frequency gravitational-wave sky (from 0.1 mHz to 1 Hz), detecting and characterizing a broad variety of systems and events throughout the Universe, including the coalescences of massive black holes brought together by galaxy mergers; the inspirals of stellar-mass black holes and compact stars into central galactic black holes; several millions of ultra-compact binaries, both detached and mass transferring, in the Galaxy; and possibly unforeseen sources such as the relic gravitational-wave radiation from the early Universe. eLISA's high signal-tonoise measurements will provide new insight into the structure and history of the Universe, and they will test general relativity in its strong-field dynamical regime.

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Section: Compact Binaries In the Galaxymentioning

confidence: 99%

Low-frequency gravitational-wave science with eLISA/NGO

Amaro-Seoane¹,

Aoudia²,

Babak³

et al. 2012

Class. Quantum Grav.

518

567

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“…Third, DWDs represent guaranteed sources for the LISA mission, and will dominate the low frequency gravitational wave band from mHz to a few Hz (e.g. Evans et al 1987;Lipunov & Postnov 1987;Hils et al 1990;Nelemans et al 2001b;Marsh 2011). Finally, detached DWD binaries with orbital periods in the range from one hour to a few minutes are particularly suitable for studying the physics of tides, a phenomenon directly related to the WD internal properties.…”

Section: E-mail:korol@strwleidenunivnlmentioning

confidence: 99%

Prospects for detection of detached double white dwarf binaries with Gaia, LSST and LISA

Korol

Rossi

Groot

et al. 2017

Monthly Notices of the Royal Astronomical Society

203

229

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Double white dwarf (DWD) binaries are expected to be very common in the Milky Way, but their intrinsic faintness challenges the detection of these systems. Currently, only a few tens of detached DWDs are know. Such systems offer the best chance of extracting the physical properties that would allow us to address a wealth of outstanding questions ranging from the nature of white dwarfs, over stellar and binary evolution to mapping the Galaxy. In this paper we explore the prospects for detections of ultra-compact (with binary separations of a few solar radii or less) detached DWDs in: 1) optical radiation with Gaia and the LSST and 2) gravitational wave radiation with LISA. We show that Gaia, LSST and LISA have the potential to detect respectively around a few hundreds, a thousand, and 25 thousand DWD systems. Moreover, Gaia and LSST data will extend by respectively a factor of two and seven the guaranteed sample of binaries detected in electromagnetic and gravitational wave radiation, opening the era of multi-messenger astronomy for these sources.

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“…Another mechanism is a common envelope induced by binary interactions (Iben & Livio 1993;Marsh et al 1995), making extremely low mass (ELM) He WDs (M He < 0.20 M or so) when the interaction occurs at the base of the RGB (see van Kerkwijk et al 1996). These ELM He WDs were first seen as companions to millisecond pulsars (e.g., Bassa et al 2006) or in high proper motion catalogs (Kawka et al 2006;Kawka & Vennes 2009), but the advent of the Sloan Digital Sky Survey (Eisenstein et al 2006) and other surveys revealed many additional ELM WDs (Kilic et al 2007b(Kilic et al , 2010b(Kilic et al , 2011c(Kilic et al , 2012Badenes et al 2009;Mullally et al 2009;Marsh et al 2011;Steinfadt et al 2010b;Parsons et al 2011;Marsh 2011;Brown et al 2011b;Vennes et al 2011, and Figure 1). ELM WDs were predicted to possess stably burning H envelopes (M env ∼ 10 −3 -10 −2 M ) that keep them bright for Gyr (Serenelli et al 2002;Panei et al 2007), and this has certainly aided the recent detections Brown et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Orbital Evolution of Compact White Dwarf Binaries

Kaplan

Bildsten

Steinfadt

2012

ApJ

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The newfound prevalence of extremely low mass (ELM, M He < 0.2 M ) helium white dwarfs (WDs) in tight binaries with more massive WDs has raised our interest in understanding the nature of their mass transfer. Possessing small (M env ∼ 10 −3 M ) but thick hydrogen envelopes, these objects have larger radii than cold WDs and so initiate mass transfer of H-rich material at orbital periods of 6-10 minutes. Building on the original work of D'Antona et al., we confirm the 10 6 yr period of continued inspiral with mass transfer of H-rich matter and highlight the fact that the inspiraling direct-impact double WD binary HM Cancri likely has an ELM WD donor. The ELM WDs have less of a radius expansion under mass loss, thus enabling a larger range of donor masses that can stably transfer matter and become a He mass transferring AM CVn binary. Even once in the long-lived AM CVn mass transferring stage, these He WDs have larger radii due to their higher entropy from the prolonged H-burning stage.

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Double white dwarfs and LISA

Cited by 79 publications

References 69 publications

Low-frequency gravitational-wave science with eLISA/NGO

Low-frequency gravitational-wave science with eLISA/NGO

Prospects for detection of detached double white dwarf binaries with Gaia, LSST and LISA

Orbital Evolution of Compact White Dwarf Binaries

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