High-Speed Photometry of the Disintegrating Planetesimals at Wd1145+017: Evidence for Rapid Dynamical Evolution

Gänsicke, B. T.; Aungwerojwit, A.; Marsh, T. R.; Dhillon, V. S.; Sahman, D. I.; Veras, Dimitri; Farihi, Jay; Chote, P.; Ashley, R. P.; Arjyotha, S.; Rattanasoon, S.; Littlefair, S. P.; Pollacco, D.; Burleigh, M. R.

doi:10.3847/2041-8205/818/1/l7

Cited by 138 publications

(154 citation statements)

References 44 publications

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“…Subsequent passes further degrade the debris and it eventually embodies a disc geometry. Vanderburg et al (2015) have recently identified the first disintegrating asteroid around the dusty WD 1145+017 (see also Gänsicke et al 2016;Rappaport et al 2016), providing support to this interpretation. The signature of a disc orbiting a WD is excess emission in the infrared due to the reprocessed light from this dust.…”

Section: Introductionmentioning

confidence: 57%

Remnant planetary systems around bright white dwarfs

Barber

Belardi

Kilic

et al. 2016

Mon. Not. R. Astron. Soc.

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We cross-correlate several sources of archival photometry for 1265 bright (V ∼ 16 mag) white dwarfs (WDs) with available high signal-to-noise spectroscopy. We find 381 WDs with archival Spitzer+IRAC data and investigate this subsample for infrared excesses due to circumstellar dust. This large data set reveals 15 dusty WDs, including three new debris discs and the hottest WD known to host dust (WD 0010+280). We study the frequency of debris discs at WDs as function of mass. The frequency peaks at 12.5 per cent for 0.7-0.75 M WDs (with 3 M main-sequence star progenitors) and falls off for stars more massive than this, which mirrors predicted planet occurrence rates for stars of different masses.

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Section: Introductionmentioning

confidence: 57%

Remnant planetary systems around bright white dwarfs

Barber

Belardi

Kilic

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Previous observation-based analyses suggested that WD 1145+017 may be currently accreting at a rate significantly higher than inferred to be ongoing for any polluted white dwarf, and up to 10 12 g s −1 (Xu et al 2016;Gänsicke et al 2016;Rappaport et al 2016). This rate is ∼ 10 2 times higher than the steady-state inference from the heavy elements in the stellar atmosphere, and ∼ 10 3 times higher than any instantaneous rate inferred via a steady-state regime calculation.…”

Section: Introductionmentioning

confidence: 99%

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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“…Recently, Vanderburg et al (2015) have identified a cloud of debris in uri.mal@tx.technion.ac.il˜˜˜˜hperets@physics.technion.ac.il the process of disintegrating (Gaensicke et al 2015;Xu et al 2016). …”

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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High-Speed Photometry of the Disintegrating Planetesimals at Wd1145+017: Evidence for Rapid Dynamical Evolution

Cited by 138 publications

References 44 publications

Remnant planetary systems around bright white dwarfs

Remnant planetary systems around bright white dwarfs

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

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