A planetesimal orbiting within the debris disc around a white dwarf star

Manser, Christopher J.; Gänsicke, B. T.; Eggl, Siegfried; Hollands, Mark; Izquierdo, Paula; Koester, D.; Landstreet, J. D.; Lyra, Wladimir; Marsh, T. R.; Meru, Farzana; Mustill, Alexander J.; Rodríguez‐Gil, P.; Toloza, Odette; Veras, Dimitri; Wilson, D. J.; Burleigh, M. R.; Davies, Melvyn B.; Farihi, Jay; Fusillo, Nicola Gentile; Martino, D. de; Parsons, S. G.; Quirrenbach, A.; Raddi, R.; Reffert, S.; Santo, M. Del; Schreiber, M. R.; Silvotti, R.; Toonen, Silvia; Villaver, E.; Wyatt, M. C.; Xu, Siyi; Zwart, Simon Portegies

doi:10.1126/science.aat5330

Cited by 188 publications

(196 citation statements)

References 99 publications

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“…(iii) Manser et al (2019) show in their fig. S2 that the EW of the Ca triplet profiles can vary as much as 20 per cent over a few weeks to months.…”

Section: Discussionmentioning

confidence: 98%

The frequency of gaseous debris discs around white dwarfs

Manser

Gänsicke

Fusillo

et al. 2020

Monthly Notices of the Royal Astronomical Society

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1 -3 per cent of white dwarfs are orbited by planetary dusty debris detectable as infrared emission in excess above the white dwarf flux. In a rare subset of these systems, a gaseous disc component is also detected via emission lines of the Ca 8600 Å triplet, broadened by the Keplerian velocity of the disc. We present the first statistical study of the fraction of debris discs containing detectable amounts of gas in emission at white dwarfs within a magnitude and signal-to-noise limited sample. We select 7705 single white dwarfs spectroscopically observed by the Sloan Digital Sky Survey (SDSS) and Gaia with magnitudes g 19. We identify five gaseous disc hosts, all of which have been previously discovered. We calculate the occurrence rate of a white dwarf hosting a debris disc detectable via Ca emission lines as 0.067 ± 0.042 0.025 per cent. This corresponds to an occurrence rate for a dusty debris disc to have an observable gaseous component in emission as 4 ± 4 2 per cent. Given that variability is a common feature of the emission profiles of gaseous debris discs, and the recent detection of a planetesimal orbiting within the disc of SDSS J122859.93+104032.9, we propose that gaseous components are tracers for the presence of planetesimals embedded in the discs and outline a qualitative model. We also present spectroscopy of the Ca triplet 8600 Å region for 20 white dwarfs hosting dusty debris discs in an attempt to identify gaseous emission. We do not detect any gaseous components in these 20 systems, consistent with the occurrence rate that we calculated.

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“…(iii) Manser et al (2019) show in their fig. S2 that the EW of the Ca triplet profiles can vary as much as 20 per cent over a few weeks to months.…”

Section: Discussionmentioning

confidence: 98%

The frequency of gaseous debris discs around white dwarfs

Manser

Gänsicke

Fusillo

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…More likely, we would require to repeat our hybrid simulations albeit utilizing SPH formulations that incorporate internal strength. Previous studies tentatively argue that an object held together by internal strength could indeed avoid disruption (Bear & Soker 2013;Brown et al 2017;Manser et al 2019). The hybrid model therefore has the potential to identify the most likely parent-objects leading to the initial formation of a comparable iron core and its accompanying disc, which would later evolve to give rise to the SDSS J122859.93+104032 observables.…”

Section: Producing the Possible Intact Planet Core Of Sdss J1228+1040?mentioning

confidence: 93%

Tidal disruption of planetary bodies by white dwarfs – II. Debris disc structure and ejected interstellar asteroids

Malamud

Perets

2020

Monthly Notices of the Royal Astronomical Society

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We make use of a new hybrid method to simulate the long-term, multiple-orbit disc formation through tidal disruptions of rocky bodies by white dwarfs, at high-resolution and realistic semi-major axis. We perform the largest-yet suite of simulations for dwarf and terrestrial planets, spanning four orders of magnitude in mass, various pericentre distances and semi-major axes between 3 AU and 150 AU. This large phase space of tidal disruption conditions has not been accessible through the use of previous codes. We analyse the statistical and structural properties of the emerging debris discs, as well as the ejected unbound debris contributing to the population of interstellar asteroids. Unlike previous tidal disruption studies of small asteroids which form ring-like structures on the original orbit, we find that the tidal disruption of larger bodies usually forms dispersed structures of interlaced elliptic eccentric annuli on tighter orbits. We characterize the (typically power-law) size-distribution of the ejected interstellar bodies as well as their composition, rotation velocities and ejection velocities. We find them to be sensitive to the depth (impact parameter) of the tidal disruption. Finally, we briefly discuss possible implications of our results in explaining the peculiar variability of Tabby's star, the origin of the transit events of ZTF J0139+5245 and the formation of a planetary core around SDSS J1228+1040.

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“…Hence, in this paper we also consider water-rich bodies. Finally, one polluted white dwarf was recently shown to be orbited by a ferrous core fragment (Manser et al 2019), indicating the importance of modelling iron-rich bodies, which we also consider here.…”

Section: Fates Of Planetary Systemsmentioning

confidence: 89%

“…The flexibility and speed of the Kurosawa & Takada (2019) formalism facilitates the study of white dwarf planetary systems because of their potential to harbour a wide variety of objects and architectures. Extending the formalism to account for very high speed impacts (> 100 km/s) and objects of high internal strength could then be applicable to impacts which occur just outside the white dwarf Roche radius, and for objects like the high-strength exo-asteroid discovered by Manser et al (2019). Because tidal interactions can quickly alter orbits (Veras et al 2019b;Veras & Wolszczan 2019;Veras & Fuller 2019, 2020, the same target might experience different impact regimes over short timescales relative to the white dwarf cooling age.…”

Section: Discussionmentioning

confidence: 99%

Generating metal-polluting debris in white dwarf planetary systems from small-impact crater ejecta

Veras

Kurosawa

2020

Monthly Notices of the Royal Astronomical Society

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Metal pollution in white dwarf photospheres originates from the accretion of some combination of planets, moons, asteroids, comets, boulders, pebbles and dust. When large bodies reside in dynamically stagnant locations -unable themselves to pollute nor even closely approach the white dwarf -then smaller reservoirs of impact debris may become a complementary or the primary source of metal pollutants. Here, we take a first step towards exploring this possibility by computing limits on the recoil mass that escapes the gravitational pull of the target object following a single impact onto an atmosphere-less surface. By considering vertical impacts only with the full-chain analytical prescription from Kurosawa & Takada (2019), we provide lower bounds for the ejected mass for basalt, granite, iron and water-rich target objects across the radii range 10 0−3 km. Our use of the full-chain prescription as opposed to physical experiments or hydrocode simulations allows us to quickly sample a wide range of parameter space appropriate to white dwarf planetary systems. Our numerical results could be used in future studies to constrain freshly-generated small debris reservoirs around white dwarfs given a particular planetary system architecture, bombardment history, and impact geometries.

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A planetesimal orbiting within the debris disc around a white dwarf star

Cited by 188 publications

References 99 publications

The frequency of gaseous debris discs around white dwarfs

The frequency of gaseous debris discs around white dwarfs

Tidal disruption of planetary bodies by white dwarfs – II. Debris disc structure and ejected interstellar asteroids

Generating metal-polluting debris in white dwarf planetary systems from small-impact crater ejecta

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