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

Bear, Ealeal; Soker, Noam

doi:10.1093/mnras/stv921

Cited by 44 publications

(17 citation statements)

References 104 publications

(146 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Large substellar bodies. Bear & Soker [ 289 ] indicated that while the envelope of a massive planet that is being destroyed may form a gaseous disc, the rocky fragments could represent small planets that then migrate within the disc; Bear & Soker [ 290 ] made a similar suggestion. Alternatively, Guillochon et al [ 291 ] and Liu et al [ 292 ] intimated that a first-generation planet may be transformed into a second-generation planet by being tidally disrupted.…”

Section: Formation From Stellar Fallbackmentioning

confidence: 99%

“…A formulation which includes the internal strength of the SB is (rearranged from eqn 8 of [ 290 ]):

where γ SB is the critical tensile strength of the SB that is disrupting. For a strengthless SB, which is representative of many ‘rubble pile’ Solar system asteroids, this equation reduces to r t ≈1.26 R ★ ( ρ ★ / ρ SB ) 1/3 .…”

Section: White Dwarf Disc Formation From First-generation Substellar mentioning

confidence: 99%

“…Bear & Soker [ 294 ] made a comparison with dwarf novae (see their table 1), which also create outbursts. Bear & Soker [ 290 ] proposed that young, hot WDs should ionize nebulae formed from an episode of AGB reincarnation due to engulfment of planetary hydrogen. Fossati et al [ 143 ] suggested that polarimetry can be used to detect non-transiting WD habitable zone planets because the signal would be 2–5 orders of magnitude larger than for habitable planets around typical M-dwarf to Sun-like stars.…”

Section: Future Directionsmentioning

confidence: 99%

See 2 more Smart Citations

Post-main-sequence planetary system evolution

2016

View full text Add to dashboard Cite

The fates of planetary systems provide unassailable insights into their formation and represent rich cross-disciplinary dynamical laboratories. Mounting observations of post-main-sequence planetary systems necessitate a complementary level of theoretical scrutiny. Here, I review the diverse dynamical processes which affect planets, asteroids, comets and pebbles as their parent stars evolve into giant branch, white dwarf and neutron stars. This reference provides a foundation for the interpretation and modelling of currently known systems and upcoming discoveries.

show abstract

Section: Formation From Stellar Fallbackmentioning

confidence: 99%

“…A formulation which includes the internal strength of the SB is (rearranged from eqn 8 of [ 290 ]):

Section: White Dwarf Disc Formation From First-generation Substellar mentioning

confidence: 99%

Section: Future Directionsmentioning

confidence: 99%

See 1 more Smart Citation

Post-main-sequence planetary system evolution

2016

View full text Add to dashboard Cite

show abstract

“…Regardless of these uncertainties, transit signatures strongly suggest that dust is emanating from the bodies, and Roche radius computations (e.g. based on equations and discussion from Murray & Dermott 1999;Cordes & Shannon 2008;Veras et al 2014b;Bear & Soker 2015) affirm that the bodies are highly likely to be currently disintegrating.…”

Section: Introductionmentioning

confidence: 99%

Dynamical mass and multiplicity constraints on co-orbital bodies around stars

Veras

Marsh

Gänsicke

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Objects transiting near or within the disruption radius of both main-sequence (e.g. KOI 1843) and white dwarf (WD 1145+017) stars are now known. Upon fragmentation or disintegration, these planets or asteroids may produce co-orbital configurations of nearly equal mass objects. However, as evidenced by the co-orbital objects detected by transit photometry in the WD 1145+017 system, these bodies are largely unconstrained in size, mass, and total number (multiplicity). Motivated by potential future similar discoveries, we perform N-body simulations to demonstrate if and how debris masses and multiplicity may be bounded due to second-to-minute deviations and the resulting accumulated phase shifts in the osculating orbital period amongst multiple co-orbital equal point masses. We establish robust lower and upper mass bounds as a function of orbital period deviation, but find the constraints on multiplicity to be weak. We also quantify the fuzzy instability boundary, and show that mutual collisions occur in less than 5, 10, and 20 per cent of our simulations for masses of 10 21 , 10 22 , and 10 23 kg. Our results may provide useful initial rough constraints on other stellar systems with multiple co-orbital bodies.

show abstract

“…The following spherical forces are similar in form to those presented in BVG17 and Bear & Soker (2015),…”

Section: Shape Model Comparisonmentioning

confidence: 84%

White dwarf planetary debris dependence on physical structure distributions within asteroid belts

McDonald

Veras

2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

White dwarfs which exhibit transit signatures of planetary debris and accreted planetary material provide exceptional opportunities to probe the material composition and dynamical structure of planetary systems. Although previous theoretical work investigating the role of minor body disruption around white dwarfs has focussed on spherical bodies, Solar System asteroids can be more accurately modelled as triaxial ellipsoids. Here we present an analytical framework to identify the type of disruption (tidal fragmentation, total sublimation or direct impact) experienced by triaxial asteroids approaching white dwarfs on extremely eccentric (e ∼ 1) orbits. This framework is then used to identify the outcomes for simplified Main belt analogues of 100 bodies across five different white dwarf temperatures. We also present an empirical relationship between cooling age and effective temperature for both DA and DB white dwarfs to identify the age of the white dwarfs considered here. We find that using a purely spherical shape model can underestimate the physical size and radial distance at which an asteroid is subjected to complete sublimation, and these differences increase with greater elongation of the body. Contrastingly, fragmentation always occurs in the largest semi-axis of a body and so can be modelled by a sphere of that radius. Both fragmentation and sublimation are greatly affected by the body’s material composition, and hence by the composition of their progenitor asteroid belts. The white dwarf temperature, and hence cooling age, can affect the expected debris distribution: higher temperatures sublimate large elongated asteroids, and cooler temperatures accommodate more direct impacts.

show abstract

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

Cited by 44 publications

References 104 publications

Post-main-sequence planetary system evolution

Post-main-sequence planetary system evolution

Dynamical mass and multiplicity constraints on co-orbital bodies around stars

White dwarf planetary debris dependence on physical structure distributions within asteroid belts

Contact Info

Product

Resources

About