- ID:
- ivo://CDS.VizieR/J/A+A/502/391
- Title:
- WASP-13b photometry and radial velocities
- Short Name:
- J/A+A/502/391
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of WASP-13b, a low-mass M_p_=0.46^+0.06^_-0.05_ M_J_ transiting exoplanet with an orbital period of 4.35298+/-0.00004days. The transit has a depth of 9mmag, and although our follow-up photometry does not allow us to constrain the impact parameter well (0<b<0.46), with radius in the range R_p_~1.06-1.21R_J_ the location of WASP-13b in the mass-radius plane is nevertheless consistent with H/He-dominated, irradiated, low core mass and core-free theoretical models. The G1V host star is similar to the Sun in mass M_*_=1.03^+0.11^_-0.09_M_{sun}_ and metallicity ([M/H]=0.0+/-0.2, but is possibly older (8.5^+5.5^_-4.9_Gyr).
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Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/531/A60
- Title:
- WASP-31b photometry and radial velocities
- Short Name:
- J/A+A/531/A60
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of the low-density, transiting giant planet WASP-31b. The planet is 0.48 Jupiter masses and 1.55 Jupiter radii. It is in a 3.4-day orbit around a metal-poor, late-F-type, V=11.7 dwarf star, which is a member of a common proper motion pair. In terms of its low density, WASP-31b is second only to WASP-17b, which is a more highly irradiated planet of similar mass.
- ID:
- ivo://CDS.VizieR/J/A+A/562/L3
- Title:
- WASP-103b radial velocities and light curves
- Short Name:
- J/A+A/562/L3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of WASP-103 b, a new ultra-short-period planet (P=22.2h) transiting a 12.1 V-magnitude F8-type main-sequence star (1.22+/-0.04M_{sun}_, 1.44_-0.03_^+0.05^R_{sun}_, Teff=6110+/-160K). WASP-103 b is significantly more massive (1.49+/-0.09M_Jup_) and larger (1.53_-0.07_^+0.05^R_Jup_) than Jupiter. Its large size and extreme irradiation (~9x10^9^erg/s/cm2) make it an exquisite target for a thorough atmospheric characterization with existing facilities. Furthermore, its orbital distance is less than 20% larger than its Roche radius, meaning that it might be significantly distorted by tides and might experience mass loss through Roche-lobe overflow. It thus represents a new key object for understanding the last stage of the tidal evolution of hot Jupiters.
- ID:
- ivo://CDS.VizieR/J/A+A/542/A4
- Title:
- WASP-43b thirty eclipses
- Short Name:
- J/A+A/542/A4
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present twenty-three transit light curves and seven occultation light curves for the ultra-short period planet WASP-43 b, in addition to eight new measurements of the radial velocity of the star. Thanks to this extensive data set, we improve significantly the parameters of the system.
- ID:
- ivo://CDS.VizieR/J/MNRAS/445/1114
- Title:
- WASP-69b, WASP-70Ab and WASP-84b
- Short Name:
- J/MNRAS/445/1114
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of the transiting exoplanets WASP-69b, WASP-70Ab and WASP-84b, each of which orbits a bright star (V~10). WASP-69b is a bloated Saturn-mass planet (0.26M_Jup_, 1.06R_Jup_) in a 3.868-d period around an active, ~1-Gyr, mid-K dwarf. ROSAT detected X-rays 60+/-27" from WASP-69. If the star is the source then the planet could be undergoing mass-loss at a rate of ~10^12^g/s. This is one to two orders of magnitude higher than the evaporation rate estimated for HD 209458b and HD 189733b, both of which have exhibited anomalously large Lyman {alpha} absorption during transit. WASP-70Ab is a sub-Jupiter-mass planet (0.59M_Jup_, 1.16R_Jup_) in a 3.713-d orbit around the primary of a spatially resolved, 9-10-Gyr, G4+K3 binary, with a separation of 3.3 arcsec ( >=800AU). WASP-84b is a sub-Jupiter-mass planet (0.69M_Jup_, 0.94R_Jup_) in an 8.523-d orbit around an active, ~1-Gyr, early-K dwarf. Of the transiting planets discovered from the ground to date, WASP-84b has the third-longest period. For the active stars WASP-69 and WASP-84, we pre-whitened the radial velocities using a low-order harmonic series. We found that this reduced the residual scatter more than did the oft-used method of pre-whitening with a fit between residual radial velocity and bisector span. The system parameters were essentially unaffected by pre-whitening.
- ID:
- ivo://CDS.VizieR/J/A+A/531/A24
- Title:
- WASP-23 photometric and radial velocity data
- Short Name:
- J/A+A/531/A24
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the discovery of a new transiting planet in the southern hemisphere. It was found by the WASP-south transit survey and confirmed photometrically and spectroscopically by the 1.2m Swiss Euler telescope, LCOGT 2m Faulkes South Telescope, the 60cm TRAPPIST telescope, and the ESO 3.6m telescope. The orbital period of the planet is 2.94 days. We find that it is a gas giant with a mass of 0.88+/-0.10M_J_ and an estimated radius of 0.96+/-0.05R_J_. We obtained spectra during transit with the HARPS spectrograph and detect the Rossiter-McLaughlin effect despite its small amplitude.
- ID:
- ivo://CDS.VizieR/J/MNRAS/473/3241
- Title:
- White dwarfs in SDSS Stripe 82
- Short Name:
- J/MNRAS/473/3241
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Binary evolution theory predicts that accreting white dwarfs with substellar companions dominate the Galactic population of cataclysmic variables (CVs). In order to test these predictions, it is necessary to identify these systems, which may be difficult if the signatures of accretion become too weak to be detected. The only chance to identify such 'dead' CVs is by exploiting their close binary nature. We have therefore searched the Sloan Digital Sky Survey (SDSS) Stripe 82 area for apparently isolated white dwarfs that undergo eclipses by a dark companion. We found no such eclipses in either the SDSS or Palomar Transient Factory data sets among our sample of 2264 photometrically selected white dwarf candidates within Stripe 82. This null result allows us to set a firm upper limit on the space density, {rho}0, of dead CVs. In order to determine this limit, we have used Monte Carlo simulations to fold our selection criteria through a simple model of the Galactic CV distribution. Assuming a T_WD_=7500K, the resulting 2{sigma} limit on the space density of dead CVs is {rho}0<~2x10^-5^pc^-3^, where TWD is the typical effective temperature of the white dwarf in such systems.
- ID:
- ivo://CDS.VizieR/J/ApJS/224/37
- Title:
- White-light flares on close binaries from Kepler
- Short Name:
- J/ApJS/224/37
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Based on Kepler data, we present the results of a search for white light flares on 1049 close binaries. We identify 234 flare binaries, of which 6818 flares are detected. We compare the flare-binary fraction in different binary morphologies ("detachedness"). The result shows that the fractions in over-contact and ellipsoidal binaries are approximately 10%-20% lower than those in detached and semi-detached systems. We calculate the binary flare activity level (AL) of all the flare binaries, and discuss its variations along the orbital period (P_orb_) and rotation period (P_rot_, calculated for only detached binaries). We find that the AL increases with decreasing P_orb_ or P_rot_, up to the critical values at P_orb_~3 days or P_rot_~1.5 days, and thereafter the AL starts decreasing no matter how fast the stars rotate. We examine the flaring rate as a function of orbital phase in two eclipsing binaries on which a large number of flares are detected. It appears that there is no correlation between flaring rate and orbital phase in these two binaries. In contrast, when we examine the function with 203 flares on 20 non-eclipse ellipsoidal binaries, bimodal distribution of amplitude-weighted flare numbers shows up at orbital phases 0.25 and 0.75. Such variation could be larger than what is expected from the cross section modification.
- ID:
- ivo://CDS.VizieR/J/ApJS/237/28
- Title:
- WISE catalog of periodic variable stars
- Short Name:
- J/ApJS/237/28
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have compiled the first all-sky mid-infrared variable-star catalog based on Wide-field Infrared Survey Explorer five-year survey data. Requiring more than 100 detections for a given object, 50282 carefully and robustly selected periodic variables are discovered, of which 34769 (69%) are new. Most are located in the Galactic plane and near the equatorial poles. A method to classify variables based on their mid-infrared light curves is established using known variable types in the General Catalog of Variable Stars. Careful classification of the new variables results in a tally of 21427 new EW-type eclipsing binaries, 5654 EA-type eclipsing binaries, 1312 Cepheids, and 1231 RR Lyrae. By comparison with known variables available in the literature, we estimate that the misclassification rate is 5% and 10% for short- and long- period variables, respectively. A detailed comparison of the types, periods, and amplitudes with variables in the Catalina catalog shows that the independently obtained classifications parameters are in excellent agreement. This enlarged sample of variable stars will not only be helpful to study Galactic structure and extinction properties, but can also be used to constrain stellar evolution theory and provide potential candidates for the James Webb Space Telescope.
- ID:
- ivo://CDS.VizieR/J/MNRAS/437/185
- Title:
- W UMa-type contact binaries ages and masses
- Short Name:
- J/MNRAS/437/185
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Recently, our understanding of the origin of W UMa-type contact binaries has become clearer. Initial masses of their components were successfully estimated by Yildiz and Dogan using a new method mainly based on observational properties of overluminous secondary components. In this paper, we continue to discuss the results and make computations for age and orbital evolution of these binaries. It is shown that the secondary mass, according to its luminosity, also successfully predicts the observed radius. While the current mass of the primary component is determined by initial masses, the current secondary mass is also a function of initial angular momentum. We develop methods to compute the age of A- and W-subtype W UMa-type contact binaries in terms of initial masses and mass according to the luminosity of the secondaries. Comparisons of our results with the mean ages from kinematic properties of these binaries and data pertaining to contact binaries in open and globular clusters have increased our confidence on this method. The mean ages of both A- and W-subtype contact binaries are found as 4.4 and 4.6Gyr, respectively. From kinematic studies, these ages are given as 4.5 and 4.4Gyr, respectively. We also compute orbital properties of A-subtype contact binaries at the time of the first overflow. Initial angular momentum of these binaries is computed by comparing them with the well-known detached binaries. The angular momentum loss rate derived in the present study for the detached phase is in very good agreement with the semi-empirical rates available in the literature. In addition to the limitations on the initial masses of W UMa-type contact binaries, it is shown that the initial period of these binaries is less than about 4.45d.
