[PDF] Top 20 A Brown Dwarf Mass Donor in an Accreting Binary

... the donor star in these systems remains a challenge, it is possible to measure the mass and radius of the donor in eclipsing ...the binary, and in particular the masses of the white ... See full document

... white dwarf, as well as the broad, double-peaked emission lines from the accretion disc, which are characteristic of high-inclination systems (Horne & Marsh ...white dwarf and a de- generate helium ... See full document

... a binary system that is composed of a brown dwarf and a solar- type ...low mass ratio between the lens components was found from  analyses of anomalous events detected in the 2014 ... See full document

... gravity, mass, radius, field strength and configuration and cool- ing ...the brown dwarf would also allow investigation of the effects of ...white dwarf plus heated polar ... See full document

... carbon mass fraction & ...an accreting neutron star yield far too little carbon to ignite a su- ...carbon mass fraction at the base of the accreted layer “by hand,” with little physical motiva- ... See full document

... low mass companions to white dwarfs (WDs) probes high mass ratio binary formation and evolution, includ- ing the known deficit of brown dwarf (BD) companions to main-sequence stars ... See full document

... a binary system MOA- 2012-BLG-006L with a mass ratio of ...the mass of the objects, rather than their ...low- mass companion to the faint host is out of reach of current tech- .../ ... See full document

... a donor that is partially degenerate to some degree. The ‘white dwarf channel’ (Nelemans et ...temperature donor in their formulation, but Deloye et ...the donor is a low-mass, ... See full document

... the gas stream collides with the edge of the accretion disc, often resulting in an ‘orbital hump’ in the light curve at phases 0.6 − 1.0 due to the area of enhanced emission ro- tating into our line of sight. For an ... See full document

... a brown dwarf donor, this scenario would be four times less likely than the detection of a period bouncer ...a brown dwarf companion, a low mass ratio and hosts the coolest white ... See full document

... This dwarf is spectrally peculiar; if the object is an unresolved 900+700 K or 800+600 K binary, then our model colors indicate that g could be higher and the age would be ∼1 Gyr, more typical for a local ... See full document

... We used LROCHE , part of the LCURVE software to model the light curves (see Copperwheat et al. 2010 for a description). We sam- ple the posterior probability distributions for model parameters us- ing affine-invariant ... See full document

... compact binary systems provide a natural laboratory for studying strongly irra- diated sub-stellar ...the mass-losing secondary in these systems makes a critical, but poorly understood transition from the ... See full document

... AU) brown dwarf-brown dwarf binaries (Basri & Martín 1999; Close et ...since brown dwarfs and low-mass hydrogen-burning stars formed by ejection are al- most always ...a ... See full document

... white dwarf channel and the He star channel require two CE events, decreasing the period to shorter than that of a normal H-rich CV and reducing the total ...white dwarf donor formation channel, the ... See full document

... in binary con fi gurations, and many interesting objects such as novae, millisecond pulsars, supersoft X-ray binaries, galactic black hole binaries and SNe Ia form due to binary interactions, mainly in the ... See full document

... the brown dwarf disc ρ Oph 102 to infer a fiducial model around which we build a small grid of brown dwarf disc models, in order to model the CO, HCN, and HCO + line fluxes and the chemistry ... See full document

... white dwarf in SDSS 0138- 0016 therefore unambiguously constrain both its tempera- ture, T = 3570 +110 −80 K, and its atmospheric composition, log(He/H) = ...white dwarf is accreting from the wind of ... See full document

... be that the lack of low velocity white dwarfs in SDSS is a statistical anomaly, since the number of objects is small. In theory this would be taken account of in the analysis described above, however young stellar ... See full document

... Panels b and c (middle and lower) we see firsthand the effects of the BVS correction to the velocities. In b we see the residuals to the best fit before the BVS correction has been applied. Two clear outliers in the ... See full document