ALMA and Herschel observations of the prototype dusty and polluted white dwarf G29-38

Farihi, Jay; Wyatt, M. C.; Greaves, J. S.; Bonsor, Amy; Sibthorpe, B.; Panić, Olja

doi:10.1093/mnras/stu1545

Cited by 29 publications

(34 citation statements)

References 79 publications

(82 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Indeed, about a quarter of single WDs have considerable amounts of metals in their photosphere, that are explained by accretion of tidally disrupted planetesimals/asteroids/comets that survived through all previous evolutionary phases of the star (see e.g. Farihi et al 2014).…”

Section: Planetary Materialsmentioning

confidence: 99%

Binarity and the Abundance Discrepancy Problem in Planetary Nebulae

Corradi

García‐Rojas

Jones

et al. 2015

ApJ

100

120

View full text Add to dashboard Cite

The discrepancy between abundances computed using optical recombination lines (ORLs) and collisionally excited lines (CELs) is a major unresolved problem in nebular astrophysics. We show here that the largest abundance discrepancies are reached in planetary nebulae with close binary central stars. This is illustrated by deep spectroscopy of three nebulae with a post commonenvelope (CE) binary star. Abell 46 and Ou5 have O 2+ /H + abundance discrepancy factors larger than 50, and as high as 300 in the inner regions of Abell 46. Abell 63 has a smaller discrepancy factor around 10, but still above the typical values in ionized nebulae. Our spectroscopic analysis supports previous conclusions that, in addition to "standard" hot (T e ∼10 4 K) gas, a colder (T e ∼10 3 K) ionized component that is highly enriched in heavy elements also exists. These nebulae have low ionized masses, between 10 −3 and 10 −1 M ⊙ depending on the adopted electron densities and temperatures. Since the much more massive red-giant envelope is expected to be entirely ejected in the CE phase, the currently observed nebulae would be produced much later, in post-CE mass loss episodes when the envelope has already dispersed. These observations add constraints to the abundance discrepancy problem. Possible explanations are revised. Some are naturally linked to binarity, such as for instance high-metallicity nova ejecta, but it is difficult at this stage to depict an evolutionary scenario consistent with all the observed properties. The hypothesis that these nebulae are the result of tidal destruction, accretion and ejection of Jupiterlike planets is also introduced.Subject headings: planetary nebulae: individual (A 46, A 63, Ou5) -ISM: abundances -binaries: close -novae, cataclysmic variables -planet-star interactions

show abstract

Section: Planetary Materialsmentioning

confidence: 99%

Binarity and the Abundance Discrepancy Problem in Planetary Nebulae

Corradi

García‐Rojas

Jones

et al. 2015

ApJ

100

120

View full text Add to dashboard Cite

show abstract

“…Observing the transfer of matter from a YORP disc to a spin or tidal disc is challenging. Current capabilities are limited to detecting dust (Xu et al 2013;Farihi et al 2014), although the highly eccentric transiting material (with an eccentricity of 0.97) orbiting ZTF J0139+5245 (Vanderbosch et al 2020) may be indicative of a transfer-inprogress. This progenitor of the observed debris could have broken up due to either rotational fission or tidal disruption depending on the location of its orbital pericentre and its physical shape.…”

Section: Implications Of Resultsmentioning

confidence: 99%

“…Regarding YORP discs, observational searches for rocky debris beyond ≈ 1.0R⊙ have been carried out by Xu et al (2013) and Farihi et al (2014) for the white dwarf planetary systems GD 362 and G29-38, respectively. These searches extended to tens of au, with a correspondingly decreasing ability to constrain the mass.…”

Section: The Outer Radius Romentioning

confidence: 99%

The lifetimes of planetary debris discs around white dwarfs

Veras

Heng

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The lifetime of a planetary disc that orbits a white dwarf represents a crucial input parameter into evolutionary models of that system. Here we apply a purely analytical formalism to estimate lifetimes of the debris phase of these discs, before they are ground down into dust or are subject to sublimation from the white dwarf. We compute maximum lifetimes for three different types of white dwarf discs, formed from (i) radiative YORP break-up of exo-asteroids along the giant branch phases at 2–100 au, (ii) radiation-less spin-up disruption of these minor planets at ${\sim} 1.5\!-\!4.5\, \mathrm{R}_{\odot }$, and (iii) tidal disruption of minor or major planets within about $1.3\, \mathrm{R}_{\odot }$. We display these maximum lifetimes as a function of disc mass and extent, constituent planetesimal properties, and representative orbital excitations of eccentricity and inclination. We find that YORP discs with masses of up to 1024 kg live long enough to provide a reservoir of surviving cm-sized pebbles and m- to km-sized boulders that can be perturbed intact to white dwarfs with cooling ages of up to 10 Gyr. Debris discs formed from the spin or tidal disruption of these minor planets or major planets can survive in a steady state for up to, respectively, 1 or 0.01 Myr, although most tidal discs would leave a steady state within about 1 yr. Our results illustrate that dust-less planetesimal transit detections are plausible, and would provide particularly robust evolutionary constraints. Our formalism can easily be adapted to individual systems and future discoveries.

show abstract

“…When tidally destructed these lead to the WD pollution as discussed above (e.g., Bergfors et al 2014;Farihi et al 2014;Wilson et al 2014 and references therein).…”

Section: Introductionmentioning

confidence: 93%

Planetary systems and real planetary nebulae from planet destruction near white dwarfs

Bear

Soker

2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We suggest that tidal destruction of Earth-like and icy planets near a white dwarf (WD) might lead to the formation of one or more low-mass − Earthlike and lighter − planets in tight orbits around the WD. The formation of the new WD planetary system starts with a tidal break-up of the parent planet to planetesimals near the tidal radius of about 1R ⊙ . Internal stress forces keep the planetesimal from further tidal break-up when their radius is less than about 100 km. We speculate that the planetesimals then bind together to form new subEarth daughter-planets at a few solar radii around the WD. More massive planets that contain hydrogen supply the WD with fresh nuclear fuel to reincarnate its stellar-giant phase. Some of the hydrogen will be inflated in a large envelope. The envelope blows a wind to form a nebula that is later (after the entire envelope is lost) ionized by the hot WD. We term this glowing ionized nebula that originated from a planet a real planetary nebula (RPN). This preliminary study of daughterplanets from a planet (DPP) and the RPN scenarios are of speculative nature. More detail studies must follow to establish whether the suggested scenarios can indeed take place.

show abstract

ALMA and Herschel observations of the prototype dusty and polluted white dwarf G29-38

Cited by 29 publications

References 79 publications

Binarity and the Abundance Discrepancy Problem in Planetary Nebulae

Binarity and the Abundance Discrepancy Problem in Planetary Nebulae

The lifetimes of planetary debris discs around white dwarfs

Planetary systems and real planetary nebulae from planet destruction near white dwarfs

Contact Info

Product

Resources

About