Doppler imaging of the planetary debris disc at the white dwarf SDSS J122859.93+104032.9

Manser, Christopher J.; Gänsicke, B. T.; Marsh, T. R.; Veras, Dimitri; Koester, D.; Breedt, E.; Pala, A. F.; Parsons, S. G.; Southworth, J.

doi:10.1093/mnras/stv2603

Cited by 123 publications

(158 citation statements)

References 66 publications

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“…This paradigm is supported by multiple lines of evidence including atmospheric pollution via heavy elements (Zuckerman et al 2003;Farihi et al 2010;Koester et al 2014), infrared and optical emission from closely orbiting disks of dust and gas (Farihi 2016), and chemical abundances broadly consistent with terrestrial-like planetesimals Jura & Young 2014;Wilson et al 2016). Evidence for short-term disk evolution has been observed in gas and dust emission features, including evidence of eccentric disk precession Wilson et al 2014;Manser et al 2016). Arguably the most spectacular example of ongoing change in a white dwarf debris disk is the rapidly varying (over minutes to months) extinction observed in both photometry and spectroscopy towards WD 1145+017 (Vanderburg et al 2015;Gänsicke et al 2016;Rappaport et al 2016;Redfield et al 2017).…”

Section: Introductionmentioning

confidence: 86%

Magnetism, X-rays and accretion rates in WD 1145+017 and other polluted white dwarf systems

Farihi

Fossati

Wheatley

et al. 2017

Monthly Notices of the Royal Astronomical Society

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This paper reports circular spectropolarimetry and X-ray observations of several polluted white dwarfs including WD 1145+017, with the aim to constrain the behavior of disk material and instantaneous accretion rates in these evolved planetary systems. Two stars with previously observed Zeeman splitting, WD 0322-019 and WD 2105-820, are detected above 5σ and B z > 1 kG, while WD 1145+017, WD 1929+011, and WD 2326+049 yield (null) detections below this minimum level of confidence. For these latter three stars, high-resolution spectra and atmospheric modeling are used to obtain limits on magnetic field strengths via the absence of Zeeman splitting, finding B * < 20 kG based on data with resolving power R ≈ 40 000. An analytical framework is presented for bulk Earth composition material falling onto the magnetic polar regions of white dwarfs, where X-rays and cyclotron radiation may contribute to accretion luminosity. This analysis is applied to X-ray data for WD 1145+017, WD 1729+371, and WD 2326+049, and the upper bound count rates are modeled with spectra for a range of plasma kT = 1 − 10 keV in both the magnetic and non-magnetic accretion regimes. The results for all three stars are consistent with a typical dusty white dwarf in a steady state at 10 8 − 10 9 g s −1 . In particular, the non-magnetic limits for WD 1145+017 are found to be well below previous estimates of up to 10 , thus suggesting the star-disk system may be average in its evolutionary state, and only special in viewing geometry.

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Section: Introductionmentioning

confidence: 86%

Magnetism, X-rays and accretion rates in WD 1145+017 and other polluted white dwarf systems

Farihi

Fossati

Wheatley

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Based on several lines of arguments (Farihi et al 2010;Koester et al 2014; it is now clear that this accretion is not from the interstellar medium, and the prevailing paradigm is that it is indicative of accretion of planetary material (Debes & Sigurdsson 2002;Jura 2003;Kilic et al 2006;Jura 2008). Although only a small percentage of WDs show infrared excess consistent with a disk (Barber et al 2012;Farihi 2016), in the last decade, nearly 40 dusty disks have nevertheless been detected around polluted WDs (Rocchetto et al 2015;Farihi 2016), and less frequently disks containing gas (Wilson et al 2014;Manser et al 2016). In contrast, there is no confirmed detection of a single debris disk around an unpolluted WD (Xu et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Post-Main Sequence Evolution of Icy Minor Planets: Implications for Water Retention and White Dwarf Pollution

Malamud

Perets

2016

ApJ

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Most observations of polluted white dwarf atmospheres are consistent with accretion of water depleted planetary material. Among tens of known cases, merely two cases involve accretion of objects that contain a considerable mass fraction of water. The purpose of this study is to investigate the relative scarcity of these detections. Based on a new and highly detailed model, we evaluate the retention of water inside icy minor planets during the high luminosity stellar evolution that follows the main sequence. Our model fully considers the thermal, physical, and chemical evolution of icy bodies, following their internal differentiation as well as water depletion, from the moment of their birth and through all stellar evolution phases preceding the formation of the white dwarf. We also account for different initial compositions and formation times. Our results differ from previous studies, that have either underestimated or overestimated water retention. We show that water can survive in a variety of circumstances and in great quantities, and therefore other possibilities are discussed in order to explain the infrequency of water detections. We predict that the sequence of accretion is such that water accretes earlier, and more rapidly than the rest of the silicate disk, considerably reducing the chance of its detection in H-dominated atmospheres. In He-dominated atmospheres, the scarcity of water detections could be observationally biased. It implies that the accreted material is typically intrinsically dry, which may be the result of inside-out depopulation sequence of minor planets.

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“…In over 35 cases, polluted WDs also harbour an observable debris disc (Zuckerman & Becklin 1987;Gänsicke et al 2006;Farihi, Jura & Zuckerman 2009;Dufour et al 2012;Farihi et al 2012;Melis et al 2012;Bergfors et al 2014;Wilson et al 2014;Manser et al 2016;Rocchetto et al 2015). No known debris disc surrounds an unpolluted WD (see Xu et al 2015 for one potential exception), strongly suggesting that the known discs are accreting on to WDs.…”

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confidence: 99%

Liberating exomoons in white dwarf planetary systems

Payne¹,

Veras²,

Holman³

et al. 2016

Mon. Not. R. Astron. Soc.

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Previous studies indicate that more than a quarter of all white dwarf (WD) atmospheres are polluted by remnant planetary material, with some WDs being observed to accrete the mass of Pluto in 10 6 yr. The short sinking time-scale for the pollutants indicates that the material must be frequently replenished. Moons may contribute decisively to this pollution process if they are liberated from their parent planets during the post-main-sequence evolution of the planetary systems. Here, we demonstrate that gravitational scattering events amongst planets in WD systems easily trigger moon ejection. Repeated close encounters within tenths of planetary Hill radii are highly destructive to even the most massive, close-in moons. Consequently, scattering increases both the frequency of perturbing agents in WD systems, as well as the available mass of polluting material in those systems, thereby enhancing opportunities for collision and fragmentation and providing more dynamical pathways for smaller bodies to reach the WD. Moreover, during intense scattering, planets themselves have pericentres with respect to the WD of only a fraction of an astronomical unit, causing extreme Hill-sphere contraction, and the liberation of moons into WD-grazing orbits. Many of our results are directly applicable to exomoons orbiting planets around main-sequence stars.

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Doppler imaging of the planetary debris disc at the white dwarf SDSS J122859.93+104032.9

Cited by 123 publications

References 66 publications

Magnetism, X-rays and accretion rates in WD 1145+017 and other polluted white dwarf systems

Magnetism, X-rays and accretion rates in WD 1145+017 and other polluted white dwarf systems

Post-Main Sequence Evolution of Icy Minor Planets: Implications for Water Retention and White Dwarf Pollution

Liberating exomoons in white dwarf planetary systems

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