Planetesimals Around Stars with TESS (PAST): I. Transient Dimming of a Binary Solar Analog at the End of the Planet Accretion Era
E. Gaidos, T. Jacobs, D. LaCourse, A. Vanderburg, S. Rappaport, T. Berger, L. Pearce, A. W. Mann, L. Weiss, B. Fulton, A. Behmard, A. W. Howard, M. Ansdell, G. … 展开作者
E. Gaidos, T. Jacobs, D. LaCourse, A. Vanderburg, S. Rappaport, T. Berger, L. Pearce, A. W. Mann, L. Weiss, B. Fulton, A. Behmard, A. W. Howard, M. Ansdell, G. R. Ricker, R. K. Vanderspek, D. W. Latham, S. Seager, J. N. Winn, J. M. Jenkins
We report detection of quasi-periodic (1.5 day) dimming of HD 240779, the solar-mass primary in a 5" visual binary (also TIC 284730577), by the Transiting Exoplanet Survey Satellite. This dimming, as has been shown for other "dipper" stars, is likely due to occultation by circumstellar dust. The barycentric space motion, lithium abundance, rotation, and chromospheric emission of the stars in this system point to an age of ~125 Myr, and possible membership in the AB Doradus moving group. As such it occupies an important but poorly explored intermediate regime of stars with transient dimming between young stellar objects in star forming regions and main sequence stars, and between UX Orionis-type Ae/Be stars and M-type "dippers". HD 240779, but not its companion BD+10714B, has WISE-detected excess infrared emission at 12 and 22 microns indicative of circumstellar dust. We propose that infrared emission is produced by collisions of planetesimals during clearing of a residual disk at the end of rocky planet formation, and that quasi-periodic dimming is produced by the rapid disintegration of a 100 km planetesimal near the silicate evaporation radius. Further studies of this and similar systems will illuminate a poorly understood final phase of rocky planet formation like that which produced the inner Solar System.
Photometric monitoring by the Transiting Exoplanet Survey Satellite (TESS) has discovered not only periodic signals by transiting exoplanets but also episodic or quasi-periodic dimming around young stellar objects. The mechanisms of the dimming of these objects, so-called "dippers", are thought to be related to the property of the accretion or the structure of protoplanetary disks especially in regions close to the host star. Recently, we have created the catalog of dippers from the one year of TESS Full Frame Image (FFI) data. In this paper, we report spectral features of four newly found dip…
The Kepler-field star KIC 8462852, an otherwise apparently ordinary F3 main-sequence star, showed several highly unusual dimming events of variable depth and duration. Adding to the mystery was the discovery that KIC 8462852 faded by 14% from 1890 to 1989, as well as by another 3% over the 4 year Kepler mission. Following an initial suggestion by Wright & Sigurdsson, we propose that the secular dimming behavior is the result of the inspiral of a planetary body or bodies into KIC 8462852, which took place ~10 to 1e4 years ago (depending on the planet mass). Gravitational energy released as the …
Evidence for a giant companion orbiting Tabby's star
University of Warwick（华威大学）；Institut d’astrophysique de Paris, UMR 7095 CNRS université Pierre et Marie Curie（巴黎天体物理研究所，CNRS联合研究单位7095，皮埃尔和玛丽居里大学）；LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris（巴黎天文台恒星与星系演化实验室（LESIA），巴黎大学，PSL大学，CNRS，索邦大学，巴黎大学）
We present detailed characterization of the extremely dusty main sequence star TYC 8830 410 1. This system hosts inner planetary system dust (Tdust~300 K) with a fractional infrared luminosity of ~1%. Mid-infrared spectroscopy reveals a strong, mildy-crystalline solid-state emission feature. TYC 8830 410 1 (spectral type G9V) has a 49.5" separation M4-type companion co-moving and co-distant with it, and we estimate a system age of ~600 Myr. TYC 8830 410 1 also experiences "dipper"-like dimming events as detected by ASAS-SN, TESS, and characterized in more detail with the LCOGT. These recurring…
We investigate four young, but non-accreting, very low mass stars in Orion, which show irregular eclipses by circumstellar dust. The eclipses are not recurring periodically, are variable in depth, lack a flat bottom, and their duration is comparable to the typical timescale between eclipses. The dimming is associated with reddening consistent with dust extinction. Taken together this implies the presence of rings around these four stars, with radii ranging from 0.01 to 40 AU, comprised of optically thin dust clouds. The stars also show IR excess indicating the presence of evolved circumstellar…
Conspicuous Gas, Cryptic Dust: Spectroscopy and Chromaticity of Complex Periodic Variables
Caltech/IPAC（加州理工学院/IPAC）；Carnegie Science Observatories（卡内基科学天文台）；Department of Astronomy, Caltech（加州理工学院天文学系）；Kavli Institute for Astrophysics and Space Research, MIT（麻省理工学院卡弗里天体物理与空间研究所）
Coronal Mass Ejections from Young Suns: An Observational View through the Solar-Stellar Connection
The Hakubi Center for Advanced Research, Kyoto University（京都大学白兔高级研究中心）；Department of Physics, Kyoto University（京都大学物理系）；Heliophysics Science Division, NASA Goddard Space Flight Center（NASA戈达德太空飞行中心太阳物理学部）；Department of Physics, The Catholic University of America（美国天主教大学物理系）
Understanding the origin of planets that have formed in binary stars is fundamental to constrain theories of binary and planet formation. The planet occurrence rate in binaries with a separation $\lesssim 50$ AU is only $\sim$ one third that of wider binaries or single stars. This may indicate that a close companion has a ruinous influence on planet formation, because it can truncate the protoplanetary disc and pump up planetesimals eccentricity and collision probability. Nevertheless, observations have revealed a few of these systems, which challenge current planet formation theories. Dynamic…
While it is well established that giant-planet occurrence rises rapidly with host star metallicity, it is not yet clear if small-planet occurrence around late-type dwarf stars depends on host star metallicity. Using the Kepler Data Release 25 planet candidate list and its completeness data products, we explore planet occurrence as a function of metallicity in the Kepler field's late-type dwarf stellar population. We find that planet occurrence increases with metallicity for all planet radii $R_{\mathrm{p}}$ down to at least $R_{\mathrm{p}}\approx2~R_{\oplus}$ and that in the range $2~R_{\oplus…
