Survival of a brown dwarf after engulfment by a red giant star
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Citations
Common envelope evolution: where we stand and how we can move forward
Common Envelope Evolution: Where we stand and how we can move forward
Retired A Stars and Their Companions: Exoplanets Orbiting Three Intermediate-Mass Subgiants
A giant planet orbiting the ‘extreme horizontal branch’ star V 391 Pegasi
Simulating the Common Envelope Phase of a Red Giant Using SPH and Uniform Grid Codes
References
Photometric Calibration of Hydrogen- and Helium-Rich White Dwarf Models
How Dry is the Brown Dwarf Desert? Quantifying the Relative Number of Planets, Brown Dwarfs, and Stellar Companions around Nearby Sun-like Stars
Low-mass white dwarfs need friends: five new double-degenerate close binary stars
Encyclopedia of Astronomy and Astrophysics
The accretion of brown dwarfs and planets by giant stars — II. Solar-mass stars on the red giant branch
Related Papers (5)
Frequently Asked Questions (14)
Q2. What is the kinetic energy of the envelope?
Some fraction of the orbital energy released, αCE, will be deposited as kinetic energy in the envelope, which is ejected from the binary system.
Q3. What is the effect of the asymmetric heating and rotation of the brown dwarf?
The asymmetric heating and rotation of the brown dwarf will produce a small but detectable modulation of the brightness at infrared wavelengths of WD0137-349 on the orbital period (“reflection effect”).
Q4. What is the spectral type of the brown dwarf?
Since most of the current mass of the brown dwarf was accreted from the red giant in this scenario, its spectral type would imply an age similar to that of the white dwarf, i.e. about 250 Ma in the case of WD0137-349.
Q5. How long will it take to become a CV?
16 The timescale for WD0137-349 to become a CV through the loss of GWR is about 1.4Ga, at which time the orbit period will be 60 – 80 minutes.
Q6. What is the spectral type of a brown dwarf?
They then start to cool, so the spectral type of a brown dwarf, which is a measure of its temperature, is also a measure of its age.
Q7. What is the value of CE required to explain the formation of WD0137-3?
21Some models predict that planets may accrete a substantial fraction of the mass inthe red giant envelope prior to a common envelope phase, resulting in the formation of a binary with similar properties to WD0137-349.
Q8. What is the value of mcrit required to explain the formation of WD0137-3?
Simple physical arguments suggest that low mass companions to red giants will be evaporated during the common envelope phase if they are less massive than some limit mcrit.
Q9. Why is the light in the emission line offset from the centre of the binary?
A correction to the value of K2 has been applied because the light in the emission line the authors measured is offset from the centre of the companion towards the centre-of-mass of the binary.
Q10. What is the reason for the simulation of the population of pre-CVs?
This raises the possibility that some fraction of CVs with very low mass companions may have formed as the result of the evolution of binaries like WD0137-349, rather than by extensive mass loss from the companion.
Q11. What is the inclination of the orbital plane to the plane of the sky?
23 Accounting for this effect will increase the value of K2 by some fraction of the projected rotational velocity of the brown dwarf, vrotsin i, where i is the inclination of the orbital plane to the plane of the sky.
Q12. What is the mass of a brown dwarf?
12 Brown dwarfs, by definition, are not massive enough to support core hydrogen burning but do undergo a brief phase of deuterium burning soon after they form.
Q13. What is the radial velocity of the H absorption line?
The measured radial velocities of the Hα absorption line at time T are given by γ1+ K1 sin(2π[T-T0]/P), and similarly for the emission line (P is orbital period, T0 is reference time, γ1 and γ2 are the apparent mean radial velocities, K1 and K2 are the semi-amplitudes of the spectroscopic orbits).
Q14. what are the main factors that determine the mass of white dwarfs?
The main factors that determine the white dwarf mass are wellunderstood and have been tested against observations, i.e., pure hydrogen model atmospheres for moderately hot white dwarfs and the mass-radius relation for degenerate stars.