White dwarf magazine download drivers#
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Masses and orbital constraints for the OGLE-2006-BLG-109Lb,c Jupiter/Saturn analog planetary system. Discovery of a Jupiter/Saturn analog with gravitational microlensing. Keck observations confirm a super-Jupiter planet orbiting M dwarf OGLE-2005-BLG-071L. WFIRST exoplanet mass-measurement method finds a planetary mass of 39 В± 8 M for OGLE-201Lb. The lowest mass ratio planetary microlens: OGLE 2016вЂ“BLGвЂ“1195Lb. Planetary and other short binary microlensing events from the MOA short-event analysis. VISTA Variables in the Via Lactea (VVV): the public ESO near-IR variability survey of the Milky Way.

White dwarf magazine download software#

SExtractor: software for source extraction.

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Astrophysics Source Code Library record no. SWarp: resampling and co-adding FITS images together. Revisiting the microlensing event Ogle 201: a solar mass star with two cold giant planets. Confirmation of the stellar binary microlensing event, Macho 97-BLG-28. Reddening and extinction toward the galactic bulge from OGLE-III: the Inner Milky WayвЂ™s R V ~ 2.5 extinction curve. Revisiting MOA 2013-BLG-220L: a solar-type star with a cold super-Jupiter companion. Retired A stars revisited: an updated giant planet occurrence rate as a function of stellar metallicity and mass. Foretellings of RagnarГ¶k: world-engulfing asymptotic giants and the inheritance of white dwarfs. Post-main-sequence planetary system evolution. The binarity of the local white dwarf population. Know your neighborhood: a detailed model atmosphere analysis of nearby white dwarfs. MOA-2011-BLG-262Lb: a sub-Earth-mass moon orbiting a gas giant primary or a high velocity planetary system in the galactic bulge. Main sequence A, F, G, and K stars: additional high-precision measurements and empirical relations. Detecting Earth-mass planets with gravitational microlensing. Cold giant planets evaporated by hot white dwarfs. MOA 2010-blg-477lb: constraining the mass of a microlensing planet from microlensing parallax, orbital motion, and detection of blended light. On the orbits of low-mass companions to white dwarfs and the fates of the known exoplanets.

White dwarf magazine download drivers#

Unstable low-mass planetary systems as drivers of white dwarf pollution. The effect of tides on the population of PN from interacting binaries. Accretion of a giant planet onto a white dwarf. Discovery of a candidate for the coolest known brown dwarf. A giant planet candidate transiting a white dwarf. A young white dwarf companion to pulsar B1620-26: evidence for early planet formation. The effects of post-main-sequence solar mass loss on the stability of our planetary system.

Can planets survive stellar evolution? Astrophys. A planetesimal orbiting within the debris disc around a white dwarf star. A disintegrating minor planet transiting a white dwarf. Located at approximately 2.0вЂ‰kiloparsecs towards the centre of our Galaxy, it is likely toВ represent an analogue to the end stages of the Sun and Jupiter in our own Solar System. This system is evidence that planets around white dwarfs can survive the giant and asymptotic giant phases of their hostвЂ™s evolution, and supports the prediction that more than half of white dwarfs have Jovian planetary companions 13. We determine that this system contains a 0.53вЂ‰В±вЂ‰0.11 M в‰ white-dwarf host orbited by a 1.4В В±В 0.3 Jupiter-mass planet with a separation on the plane of the sky of 2.8 В± 0.5вЂ‰astronomical units, which implies a semi-major axis larger than this.

Here we report the non-detection of a main-sequence lens star in the microlensing event MOA-2010-BLG-477Lb 12 using near-infrared observations from the Keck Observatory. Simulations predict 9, 10, 11 that planets in Jupiter-like orbits around stars of в‰І8 M в‰ (solar mass)В avoid being destroyed by the strong tidal forces of their stellar host, but as yet, there has been no observational confirmation of such a survivor. Studies 1, 2 have shown that the remnants of destroyed planets and debris-disk planetesimals can survive the volatile evolution of their host stars into white dwarfs 3, 4, but few intact planetary bodies around white dwarfs have been detected 5, 6, 7, 8.