A THIRD HOT WHITE DWARF COMPANION DETECTED BYKEPLER

Abstract

We have found a system listed in the Kepler Binary Catalog (P orb = 3.273 days) that we have determined is comprised of a low-mass, thermally bloated, hot white dwarf orbiting an A star of about 2.3 M . In this work, we designate the object, KIC 10657664, simply as "KHWD3" (Kepler Hot White Dwarf 3). We use the transit depth of ∼0.66%, the eclipse depth of ∼1.9%, and regular smooth periodic variations at the orbital frequency and twice the orbital frequency to analyze the system parameters. The smooth periodic variations are identified with the classical ellipsoidal light variation (ELV) and illumination (ILL) effects, and the newly utilized Doppler boosting (DB) effect. Given the measured values of R/a and inclination angle of the binary, both the ELV and DB effects are mostly sensitive to the mass ratio, q = M 2 /M 1 , of the binary. The two effects yield values of q which are somewhat inconsistent-presumably due to unidentified systematic effects-but which nonetheless provide a quite useful set of possibilities for the mass of the white dwarf (either 0.26 ± 0.04 M or 0.37 ± 0.08 M ). All of the other system parameters are determined fairly robustly. In particular, we show that the white dwarf has a radius of 0.15 ± 0.01 R , which is extremely bloated over the radius it would have as a fully degenerate object, and an effective temperature T eff 14,500 K. Binary evolution scenarios and models for this system are discussed. We suggest that the progenitor binary was comprised of a primary of mass ∼2.2 M (the progenitor of the current hot white dwarf) and a secondary of mass ∼1.4 M (the progenitor of the current A star in the system). We compare this new system with three other white dwarfs in binaries that likely were formed via stable Roche-lobe overflow (KOI-74, KOI-81, and the inner Regulus binary).

SOPHIE velocimetry ofKeplertransit candidates

“…Consequently, both the spectroscopic and Doppler boosting methods can be used to estimate the radial velocity amplitude of stars with massive companions (see also Bloemen et al 2010). Carter et al (2010) recently announced a third transiting white dwarf detected with Kepler. In this case, the mass ratio between the white dwarf and its A-type companion is found to be inconsistent when calculated with ellipsoidal light variations or Doppler boosting.…”

The Formation of EL CVn-type Binaries

“…Similar to Fig.13 but for the WD mass distributions. The filled triangles and stars are for EL CVn-type stars (Maxted et al 2013) and Kepler objects (van Kerkwijk et al 2010;Carter, Rappaport & Fabrycky 2011;Breton et al 2012;Rappaport et al 2015), respectively. curves.…”

TWENTY-ONE NEW LIGHT CURVES OF OGLE-TR-56b: NEW SYSTEM PARAMETERS AND LIMITS ON TIMING VARIATIONS

“…This method is described in greater detail in, e.g., Carter et al (2011). Three independent chains of a million links each were combined, discarding the first 50,000 links of each chain, to avoid any potential (Table 5) are shown for the inclination (i), semimajor axis (a/R * ), planet-star radius ratio (k), total transit duration (T 14 ), full transit duration (T 23 ), and ingress/egress duration, assuming a circular orbit (T 12 = T 34 ).…”