<i>Hubble Space Telescope</i>Parallaxes of AM CVn Stars and Astrophysical Consequences

Roelofs, G.; Groot, P.; Benedict, G. F.; McArthur, B.; Steeghs, D.; Morales-Rueda, L.; Marsh, T. R.; Nelemans, G.

doi:10.1086/520491

Cited by 101 publications

(136 citation statements)

References 50 publications

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“…Together with estimates for the component masses from the absolute magnitudes this has led to estimates of the expected LISA signal that are well determined with reliable error bars ( Fig. 2 and Roelofs et al, 2007a). For the shortest periods systems the distances and component masses are not (yet) well determined enough to give well defined signal estimates.…”

Section: Verification Binariesmentioning

confidence: 84%

“…As each position in the sky is visited many times (typically around 90 times) parallax and proper motion of all objects will be determined. Only for a handful of AM CVn stars their parameters are well determined and reliable error bars can be given (Roelofs et al, 2007a), the rest are estimates. The dashed line shows the LISA sensitivity, the solid line an estimate of the Galactic foreground noise (from Nelemans et al, 2004b).…”

Section: Egaps the European Galactic Plane Survey (Egaps) Is Surveyinmentioning

confidence: 99%

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The Galactic gravitational wave foreground

Nelemans

2009

Class. Quantum Grav.

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Abstract. I present an overview of the Galactic binaries that form the foreground for the ESA/NASA Laser Interferometer Space Antenna (LISA). The currently known population is discussed, as well as current and near-future large-scale surveys that will find new systems. The astrophysics that can be done when the LISA data becomes available is presented, with particular attention to verification binaries, the overall Galactic populations, neutron star and black hole binaries and sources in globular clusters. I discuss the synergy with electro-magnetic observations and correct an error in the estimate of the number of LISA systems that can be found in the optical compared to Nelemans (2006a) and conclude that at least several hundreds of systems should be detectable.PACS numbers: 95.85. Sz, 97.80.Fk, 98.35.Ln,

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Section: Verification Binariesmentioning

confidence: 84%

Section: Egaps the European Galactic Plane Survey (Egaps) Is Surveyinmentioning

confidence: 99%

The Galactic gravitational wave foreground

Nelemans

2009

Class. Quantum Grav.

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“…The gravitational wave strain amplitude h scales with the masses of both binary components, the binary inclination, the orbital period and the distance of the system. We calculate it as described in Roelofs et al (2007) to be as high as log h = −21.5 ± 0.3; CD-30 • 11223 should therefore be one of the strongest gravitational wave sources detectable with missions like NGO/eLISA (Kilic et al 2012;Nelemans 2009). It is even more noticeable, because the presence of eclipses allows us determine its binary parameters to very high accuracy.…”

Section: Gravitational Wave Radiationmentioning

confidence: 98%

A progenitor binary and an ejected mass donor remnant of faint type Ia supernovae

Geier

Marsh

Wang

et al. 2013

A&A

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116

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Type Ia supernovae (SN Ia) are the most important standard candles for measuring the expansion history of the universe. The thermonuclear explosion of a white dwarf can explain their observed properties, but neither the progenitor systems nor any stellar remnants have been conclusively identified. Underluminous SN Ia have been proposed to originate from a so-called double-detonation of a white dwarf. After a critical amount of helium is deposited on the surface through accretion from a close companion, the helium is ignited causing a detonation wave that triggers the explosion of the white dwarf itself. We have discovered both shallow transits and eclipses in the tight binary system CD-30 • 11223 composed of a carbon/oxygen white dwarf and a hot helium star, allowing us to determine its component masses and fundamental parameters. In the future the system will transfer mass from the helium star to the white dwarf. Modelling this process we find that the detonation in the accreted helium layer is sufficiently strong to trigger the explosion of the core. The helium star will then be ejected at such high velocity that it will escape the Galaxy. The predicted properties of this remnant are an excellent match to the so-called hypervelocity star US 708, a hot, helium-rich star moving at more than 750 km s −1 , sufficient for it to leave the Galaxy. The identification of both progenitor and remnant provides a consistent picture of the formation and evolution of underluminous SNIa.

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“…The orbital period is 1029 s (Harvey et al 1998). For primary and secondary masses there are several values in discussion, with the most agreed upon being M WD ≈ 0.7 M and M 2 ≈ 0.1 M (Roelofs et al 2007). However, using synthetic spectra of a large grid of accretion-disk models (Nagel et al 2009) calculated with AD, we found the best agreement with observation for models with M WD = 0.6 M and an accretion ratė M = 1 × 10 −8 M yr −1 .…”

Section: Standard Hydrodynamic Modelmentioning

confidence: 99%

Monte Carlo radiation transfer in CV disk winds: application to the AM CVn prototype

Kusterer

Nagel

Hartmann

et al. 2013

A&A

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Context. AM CVn systems are ultracompact binaries in which a (semi-) degenerate star transfers helium-dominated matter onto a white dwarf. They are effective gravitational-wave emitters and potential progenitors of Type Ia supernovae. Aims. To understand the evolution of AM CVn systems it is necessary to determine their mass-loss rate through their radiationdriven accretion-disk wind. We constructed models to perform quantitative spectroscopy of P Cygni line profiles that were detected in UV spectra. Methods. We performed 2.5D Monte Carlo radiative transfer calculations in hydrodynamic wind structures by making use of realistic NLTE spectra from the accretion disk and by accounting for the white dwarf as an additional photon source. Results. We present first results from calculations in which LTE opacities are used in the wind model. A comparison with UV spectroscopy of the AM CVn prototype shows that the modeling procedure is potentially a good tool for determining mass-loss rates and abundances of trace metals in the helium-rich wind.

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Hubble Space TelescopeParallaxes of AM CVn Stars and Astrophysical Consequences

Cited by 101 publications

References 50 publications

The Galactic gravitational wave foreground

The Galactic gravitational wave foreground

A progenitor binary and an ejected mass donor remnant of faint type Ia supernovae

Monte Carlo radiation transfer in CV disk winds: application to the AM CVn prototype

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