DOCSLIB.ORG

Direct Imaging of an Asymmetric Debris Disk in the Hd 106906 Planetary System

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Direct Imaging of an Asymmetric Debris Disk in the Hd 106906 Planetary System The Astrophysical Journal, 814:32 (12pp), 2015 November 20 doi:10.1088/0004-637X/814/1/32 © 2015. The American Astronomical Society. All rights reserved. DIRECT IMAGING OF AN ASYMMETRIC DEBRIS DISK IN THE HD 106906 PLANETARY SYSTEM Paul G. Kalas1, Abhijith Rajan2, Jason J. Wang1, Maxwell A. Millar-Blanchaer3,30, Gaspard Duchene1,4,5, Christine Chen6, Michael P. Fitzgerald7, Ruobing Dong1, James R. Graham1, Jennifer Patience2, Bruce Macintosh8, Ruth Murray-Clay9, Brenda Matthews10, Julien Rameau11, Christian Marois10, Jeffrey Chilcote3,30, Robert J. De Rosa1, René Doyon11, Zachary H. Draper10, Samantha Lawler10, S. Mark Ammons12, Pauline Arriaga7, Joanna Bulger13, Tara Cotten14, Katherine B. Follette8, Stephen Goodsell15, Alexandra Greenbaum16, Pascale Hibon15, Sasha Hinkley17, Li-Wei Hung7, Patrick Ingraham18, Quinn Konapacky19, David Lafreniere11, James E. Larkin7, Douglas Long6, Jérôme Maire3, Franck Marchis20, Stan Metchev21,22,23, Katie M. Morzinski24, Eric L. Nielsen8,20, Rebecca Oppenheimer25, Marshall D. Perrin6, Laurent Pueyo6, Fredrik T. Rantakyrö15, Jean-Baptiste Ruffio8, Leslie Saddlemyer10, Dmitry Savransky26, Adam C. Schneider27, Anand Sivaramakrishnan6, Rémi Soummer6, Inseok Song14, Sandrine Thomas18, Gautam Vasisht28, Kimberly Ward-Duong2, Sloane J. Wiktorowicz29, and Schuyler G. Wolff6,16 1 Astronomy Department, University of California, Berkeley CA 94720-3411, USA 2 School of Earth and Space Exploration, Arizona State University, P.O. Box 871404, Tempe, AZ 85287, USA 3 Department of Astronomy & Astrophysics, University of Toronto, Toronto ON M5S 3H4, Canada 4 Université of Grenoble Alpes, IPAG, F-38000 Grenoble, France 5 CNRS, IPAG, F-38000 Grenoble, France 6 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 7 Department of Physics & Astronomy, UCLA, Los Angeles, CA 90095, USA 8 Kavli Institute for Particle Astrophysics & Cosmology, Stanford University, Stanford, CA 94305, USA 9 Department of Physics, University of California, Santa Barbara, CA 93106, USA 10 National Research Council of Canada Herzberg, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 11 Institut de Recherche sur les Exoplanetes, Département de Physique, Université de Montréal, Montréal QC H3C 3J7, Canada 12 Lawrence Livermore National Laboratory, 7000 East Avenue, Livermore, CA 94040, USA 13 Subaru Telescope, National Astronomical Observatory of Japan, 650, North Aohoku Place, Hilo, HI 96720, USA 14 Department of Physics & Astronomy, The University of Georgia, Athens, GA 30602-2451, USA 15 Gemini Observatory, Casilla 603, La Serena, Chile 16 Physics & Astronomy Department, Johns Hopkins University, Baltimore, MD 21218, USA 17 School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK 18 AURA/LSST, 950 N. Cherry Avenue, Tucson, AZ 85719, USA 19 University of California, San Diego, La Jolla, CA 92093, USA 20 SETI Institute, Carl Sagan Center, 189 Bernardo Avenue, Mountain View, CA 94043, USA 21 Physics & Astronomy Department, University of Western Ontario, London, ON N6A 3K7, Canada 22 Centre for Planetary & Space Exploration, University of Western Ontario, London, ON N6A 3K7, Canada 23 Physics & Astronomy Department, Stony Brook University, Stony Brook, NY 11794-3800, USA 24 Steward Observatory, Center for Astronomical Adaptive Optics, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA 25 American Museum of Natural History, New York, NY 10024, USA 26 Sibley School of Mechanical & Aerospace Engineering, Cornell University, Ithaca NY 14853, USA 27 University of Toledo, 2801 W. Bancroft Street, Toledo, OH 43606, USA 28 NASA Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 29 Department of Astronomy & Astrophysics, University of California, Santa Cruz, CA 95064, USA 30 Dunlap Institute for Astronomy & Astrophys., University of Toronto, Toronto ON M5S 3H4, Canada Received 2015 June 26; accepted 2015 October 8; published 2015 November 13 ABSTRACT We present the first scattered light detections of the HD 106906 debris disk using the Gemini/Gemini Planet Imager in the infrared and Hubble Space Telescope (HST)/Advanced Camera for Surveys in the optical. HD 106906 is a 13 Myr old F5V star in the Sco–Cen association, with a previously detected planet-mass candidate HD 106906b projected 650 AU from the host star. Our observations reveal a near edge-on debris disk that has a central cleared region with radius ∼50 AU, and an outer extent >500 AU. The HST data show that the outer regions are highly asymmetric, resembling the “needle” morphology seen for the HD 15115 debris disk. The planet candidate is oriented ∼21° away from the position angle of the primary’s debris disk, strongly suggesting non-coplanarity with the system. We hypothesize that HD 106906b could be dynamically involved in the perturbation of the primary’s disk, and investigate whether or not there is evidence for a circumplanetary dust disk or cloud that is either primordial or captured from the primary. We show that both the existing optical properties and near-infrared colors of HD 106906b are weakly consistent with this possibility, motivating future work to test for the observational signatures of dust surrounding the planet. Key words: circumstellar matter – infrared: stars – stars: individual (HD 106906) – techniques: high angular resolution 1 The Astrophysical Journal, 814:32 (12pp), 2015 November 20 Kalas et al. 1. INTRODUCTION band spectral mode with 25°.3 of field rotation. An additional eight 90 s exposures were collected in imaging polarimetry The Gemini Planet Imager (GPI) Exoplanet Survey is mode at four different waveplate orientations (0°, 22°.5, 45°, targeting 600 young, nearby stars to directly detect and and 67°.5; two exposures per orientation) with 7°.1 of field characterize extrasolar planets and dusty debris disks. The rotation. general observing strategy is to obtain relatively deep (∼1 hr) The spectral and polarimetry mode data were reduced using observations of young stars with the spectroscopic mode of the GPI Data Reduction Pipeline (Perrin et al. 2014). The GPI, and shorter snapshots using GPI’s dual channel imaging spectral data were dark subtracted, flexure corrected, and polarimetry mode to detect polarized light scattered by wavelength calibrated with an H-band Ar discharge lamp taken circumstellar dust grains. The scientific motivations include immediately before the science sequence. Bad pixels were quantifying the frequency and masses of Jovians from 5 to repaired in the raw 2D data, the data were assembled into 50 AU, determining the properties of their atmospheres, and datacubes, and corrected for distortion. The polarimetry data understanding their dynamical co-evolution with the planete- were dark subtracted, flexure corrected using a cross-correla- simals that replenish reservoirs of dust grains seen as debris tion method, bad pixels repaired, corrected for the lenslet disks. In particular, well-resolved debris disks typically have response using the Gemini calibration flat field lamp, and features such as central holes, azimuthal clumps, and vertical assembled into a Stokes datacube using a Mueller matrix model warps that in a single snapshot reveal key properties of each of the instrument. The instrumental polarization was subtracted system’s recent dynamical history. as described in Millar-Blanchaer et al. (2015). The Stokes Fomalhaut, HR 8799, HD 95086, and β Pic are four datacube was then converted to the radial Stokes convention prominent examples of dusty debris disks dynamically ( IQUV,,, IQ , , UV , ;Schmid et al. 2006), which associated with directly imaged planets (Kalas et al. 2008; [ ][rr ] places the tangentially (ortho-radial) and radially polarized Marois et al. 2008, 2010; Lagrange et al. 2009; Rameau et al. intensity into the Q image. Under the convention used here, 2013), but a more recent candidate for planet-disk interactions r tangentially polarized intensity results in positive values in the is HD 106906 (HIP 59960; 92 ± 6 pc; F5V; 1.5 M ; 5.6 L ; 13 Q image. ± 2 Myr; Pecaut et al. 2012). The dusty debris disk was first r In polarimetry mode, the data outside of ∼0 3 is typically discovered with a Spitzer infrared survey of 25 stars comprising dominated by the photon noise of the point-spread function Lower Centaurus Crux (Chen et al. 2005). Excess infrared (PSF) halo and detector read noise (Perrin et al. 2014). To emission in both the Spitzer MIPS 24 and 70 μm bands improve the signal to noise, we apply a Gaussian filter with correspond to L L 1.4 103 and a blackbody radius of IR FWHM = 3 pixels (42 mas; the FWHM of Gemini’s diffraction ∼20 AU (Chen et al. 2011; see also Jang-Condell et al. 2015). limited PSF in the H-band). A comoving, substellar companion (11 ± 2 M ) was Jup The initial discovery of the disk in both the spectral and subsequently discovered at a projected separation of 7 11 polarimetry mode data prompted us to re-examine the archival (654 AU) and a position angle of PA = 307°.3 (Bailey HST data obtained with the Advanced Camera for Surveys et al. 2014) using the Magellan AO system (Close et al. 2013). High Resolution Channel (ACS/HRC) coronagraph. These At such a large projected distance, a key question is whether or optical data (F606W; 2 frames of 1250 s each) were obtained not HD 106906b originally formed like a planet in a UT 2004 December 01 as part of a follow-up imaging circumstellar disk surrounding the primary and was subse- campaign to stars with Spitzer-detected infrared
Load more

Recommended publications
  • Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
    Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born.
    [Show full text]
  • Arxiv:1607.06007V1
    Accepted in ApJ A Preprint typeset using L TEX style emulateapj v. 11/12/01 THERMAL INFRARED IMAGING AND ATMOSPHERIC MODELING OF VHS J125601.92-125723.9 b: EVIDENCE FOR MODERATELY THICK CLOUDS AND EQUILIBRIUM CARBON CHEMISTRY IN A HIERARCHICAL TRIPLE SYSTEM Evan A. Rich1, Thayne Currie2, John P. Wisniewski1, Jun Hashimoto3, Timothy D. Brandt4,5, Joseph C. Carson6, Masayuki Kuzuhara7, Taichi Uyama8 Accepted in ApJ ABSTRACT We present and analyze Subaru/IRCS L′and M ′ images of the nearby M dwarf VHS J125601.92- 125723.9 (VHS 1256), which was recently claimed to have a ∼11 MJ companion (VHS 1256 b) at ∼102 au separation. Our adaptive optics images partially resolve the central star into a binary, whose components are nearly equal in brightness and separated by 0′′. 106 ± 0′′. 001. VHS 1256 b occupies nearly the same near-infrared color-magnitude diagram position as HR 8799 bcde and has a comparable L′ brightness. However, it has a substantially redder H - M ′ color, implying a relatively brighter M ′ flux density than for the HR 8799 planets and suggesting that non-equilibrium carbon chemistry may be less significant in VHS 1256 b. We successfully match the entire SED (optical through thermal infrared) for VHS 1256 b to atmospheric models assuming chemical equilibrium, models which failed to reproduce HR 8799 b at 5 µm. Our modeling favors slightly thick clouds in the companion’s atmosphere, although perhaps not quite as thick as those favored recently for HR 8799 bcde. Combined with the non-detection of lithium in the primary, we estimate that the system is at least older than 200 Myr and the masses of the stars comprising the central binary are at least 58 MJ each.
    [Show full text]
  • Constraints on the Spin Evolution of Young Planetary-Mass Companions Marta L
    Constraints on the Spin Evolution of Young Planetary-Mass Companions Marta L. Bryan1, Björn Benneke2, Heather A. Knutson2, Konstantin Batygin2, Brendan P. Bowler3 1Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, CA 91125, USA. 2Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA. 3McDonald Observatory and Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA. Surveys of young star-forming regions have discovered a growing population of planetary- 1 mass (<13 MJup) companions around young stars . There is an ongoing debate as to whether these companions formed like planets (that is, from the circumstellar disk)2, or if they represent the low-mass tail of the star formation process3. In this study we utilize high-resolution spectroscopy to measure rotation rates of three young (2-300 Myr) planetary-mass companions and combine these measurements with published rotation rates for two additional companions4,5 to provide a look at the spin distribution of these objects. We compare this distribution to complementary rotation rate measurements for six brown dwarfs with masses <20 MJup, and show that these distributions are indistinguishable. This suggests that either that these two populations formed via the same mechanism, or that processes regulating rotation rates are independent of formation mechanism. We find that rotation rates for both populations are well below their break-up velocities and do not evolve significantly during the first few hundred million years after the end of accretion. This suggests that rotation rates are set during late stages of accretion, possibly by interactions with a circumplanetary disk.
    [Show full text]
  • Direct Imaging and Spectroscopy of a Candidate Companion Below/Near
    Draft version June 13, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 DIRECT IMAGING AND SPECTROSCOPY OF A CANDIDATE COMPANION BELOW/NEAR THE DEUTERIUM-BURNING LIMIT IN THE YOUNG BINARY STAR SYSTEM, ROXS 42B Thayne Currie1, Sebastian Daemgen1, John Debes2, David Lafreniere3, Yoichi Itoh4, Ray Jayawardhana1, Thorsten Ratzka5, Serge Correia6 Draft version June 13, 2018 ABSTRACT We present near-infrared high-contrast imaging photometry and integral field spectroscopy of ROXs 42B, a binary M0 member of the 1–3 Myr-old ρ Ophiuchus star-forming region, from data collected ′′ over 7 years. Each data set reveals a faint companion – ROXs 42Bb – located ∼ 1.16 (rproj ≈ 150 AU) from the primaries at a position angle consistent with a point source identified earlier by Ratzka et al. (2005). ROXs 42Bb’s astrometry is inconsistent with a background star but consistent with a bound companion, possibly one with detected orbital motion. The most recent data set reveals a second candidate companion at ∼ 0′′. 5 of roughly equal brightness, though preliminary analysis indicates it is a background object. ROXs 42Bb’s H and Ks band photometry is similar to dusty/cloudy young, low-mass late M/early L dwarfs. K-band VLT/SINFONI spectroscopy shows ROXs 42Bb to be a cool substellar object (M8–L0; Teff ≈ 1800–2600 K), not a background dwarf star, with a spectral shape indicative of young, low surface gravity planet-mass companions. We estimate ROXs 42Bb’s mass to be 6–15 MJ , either below the deuterium burning limit and thus planet mass or straddling the deuterium-burning limit nominally separating planet-mass companions from other substellar objects.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
    exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55
    [Show full text]
  • Exoplanet Meteorology: Characterizing the Atmospheres Of
    Exoplanet Meteorology: Characterizing the Atmospheres of Directly Imaged Sub-Stellar Objects by Abhijith Rajan A Dissertation Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy Approved April 2017 by the Graduate Supervisory Committee: Jennifer Patience, Co-Chair Patrick Young, Co-Chair Paul Scowen Nathaniel Butler Evgenya Shkolnik ARIZONA STATE UNIVERSITY May 2017 ©2017 Abhijith Rajan All Rights Reserved ABSTRACT The field of exoplanet science has matured over the past two decades with over 3500 confirmed exoplanets. However, many fundamental questions regarding the composition, and formation mechanism remain unanswered. Atmospheres are a window into the properties of a planet, and spectroscopic studies can help resolve many of these questions. For the first part of my dissertation, I participated in two studies of the atmospheres of brown dwarfs to search for weather variations. To understand the evolution of weather on brown dwarfs we conducted a multi- epoch study monitoring four cool brown dwarfs to search for photometric variability. These cool brown dwarfs are predicted to have salt and sulfide clouds condensing in their upper atmosphere and we detected one high amplitude variable. Combining observations for all T5 and later brown dwarfs we note a possible correlation between variability and cloud opacity. For the second half of my thesis, I focused on characterizing the atmospheres of directly imaged exoplanets. In the first study Hubble Space Telescope data on HR8799, in wavelengths unobservable from the ground, provide constraints on the presence of clouds in the outer planets. Next, I present research done in collaboration with the Gemini Planet Imager Exoplanet Survey (GPIES) team including an exploration of the instrument contrast against environmental parameters, and an examination of the environment of the planet in the HD 106906 system.
    [Show full text]
  • 2019 Rich Evan Dissertation.Pdf
    UNIVERSITY OF OKLAHOMA GRADUATE COLLEGE THE UNIQUE GEOMETRIES AND ILLUMINATIONS OF PROTOPLANETARY DISKS AND THEIR POTENTIAL EXOPLANETS A DISSERTATION SUBMITTED TO THE GRADUATE FACULTY in partial fulfillment of the requirements for the Degree of DOCTOR OF PHILOSOPHY By Evan A. Rich Norman, Oklahoma 2019 THE UNIQUE GEOMETRIES AND ILLUMINATIONS OF PROTOPLANETARY DISKS AND THEIR POTENTIAL EXOPLANETS A DISSERTATION APPROVED FOR THE HOMER L. DODGE DEPARTMENT OF PHYSICS AND ASTRONOMY BY Dr. John Wisniewski, Chair Dr. Nathan Kaib Dr. Kieren Mullen Dr.Michael Sitko Dr. Kerry Magruder c Copyright Evan A. Rich 2019 All Rights Reserved. To my Mom and Dad who first inspired me to investigate the natural world around me and gave me the resources to succeed. And to my wife Sarah who makes all of this all worth while. iv Acknowledgements Much of the work in this dissertation could not have been done without the native Hawaiian's sharing their island and mountain with the astronomical com- munity. I would like to recognize the significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian com- munity. I am most fortunate to have the opportunity to conduct astronomical observations from their mountain. This work was performed as part of the larger SEEDS project. Specifically, I would like to acknowledge help from Dr. Thayne Currie, Dr. Misato Fukagawa, Dr. Carol Grady, Dr. Jun Hashimoto, Dr. Micheal Sitko, and Dr. John Tobin. And finally I would like to acknowledge my advisor Dr. John Wisniewski who has worked tirelessly to ensure I had every opportunity to succeed.
    [Show full text]
  • Why Do Hydrogen and Helium Migrate from Some Planets and Smaller
    Why do Hydrogen and Helium Migrate from Some Planets and Smaller Objects? Author Weitter Duckss Independent Researcher, Zadar, Croatia mail: [email protected] Project: https://www.svemir-ipaksevrti.com/ Abstract This article analyzes the processes through measuring the material incoming from the outer space onto Earth, through migrating of hydrogen and helium from our atmosphere and from other objects and through inability to detect the radioactive effects on stars and objects with melted interiorities. Habitable periods on such objects are determined through the processes. 1. Introduction The goal of the article is to give arguments, based on the existing data bases, that a constant growth of space objects, as well as their rotation and tidal forces, cause their warming up and radiation emissions, therefore making radioactive processes of fission and fusion – which are not detected on stars and other objects anyway – unnecessary. The article gives evidence of hydrogen and helium migrating towards the objects that have more mass and of temperature levels of stars being directly related to their chemical compositions and the objects in their orbits. The argumentation to support a habitable period will be derived from the natural processes of constant growth and matter gathering. 2. Why there is no radioactive emission, derived from the processes of fission and fusion, inside stars? All data bases indicate that astronomic research (or, evidence) support the existence of a constant (monotonous), omnipresent, slow gathering of matter. The processes are "more accelerated" in such part of the Universe where there is more matter gathered (in the form of nebulae, molecular clouds, etc.) during a long period of time, but gathering takes place constantly in the whole volume of the Universe as well.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 Star Distance Star Name Star Mass
    exoplanet.eu_catalog star_distance star_name star_mass Planet name mass 1.3 Proxima Centauri 0.120 Proxima Cen b 0.004 1.3 alpha Cen B 0.934 alf Cen B b 0.004 2.3 WISE 0855-0714 WISE 0855-0714 6.000 2.6 Lalande 21185 0.460 Lalande 21185 b 0.012 3.2 eps Eridani 0.830 eps Eridani b 3.090 3.4 Ross 128 0.168 Ross 128 b 0.004 3.6 GJ 15 A 0.375 GJ 15 A b 0.017 3.6 YZ Cet 0.130 YZ Cet d 0.004 3.6 YZ Cet 0.130 YZ Cet c 0.003 3.6 YZ Cet 0.130 YZ Cet b 0.002 3.6 eps Ind A 0.762 eps Ind A b 2.710 3.7 tau Cet 0.783 tau Cet e 0.012 3.7 tau Cet 0.783 tau Cet f 0.012 3.7 tau Cet 0.783 tau Cet h 0.006 3.7 tau Cet 0.783 tau Cet g 0.006 3.8 GJ 273 0.290 GJ 273 b 0.009 3.8 GJ 273 0.290 GJ 273 c 0.004 3.9 Kapteyn's 0.281 Kapteyn's c 0.022 3.9 Kapteyn's 0.281 Kapteyn's b 0.015 4.3 Wolf 1061 0.250 Wolf 1061 d 0.024 4.3 Wolf 1061 0.250 Wolf 1061 c 0.011 4.3 Wolf 1061 0.250 Wolf 1061 b 0.006 4.5 GJ 687 0.413 GJ 687 b 0.058 4.5 GJ 674 0.350 GJ 674 b 0.040 4.7 GJ 876 0.334 GJ 876 b 1.938 4.7 GJ 876 0.334 GJ 876 c 0.856 4.7 GJ 876 0.334 GJ 876 e 0.045 4.7 GJ 876 0.334 GJ 876 d 0.022 4.9 GJ 832 0.450 GJ 832 b 0.689 4.9 GJ 832 0.450 GJ 832 c 0.016 5.9 GJ 570 ABC 0.802 GJ 570 D 42.500 6.0 SIMP0136+0933 SIMP0136+0933 12.700 6.1 HD 20794 0.813 HD 20794 e 0.015 6.1 HD 20794 0.813 HD 20794 d 0.011 6.1 HD 20794 0.813 HD 20794 b 0.009 6.2 GJ 581 0.310 GJ 581 b 0.050 6.2 GJ 581 0.310 GJ 581 c 0.017 6.2 GJ 581 0.310 GJ 581 e 0.006 6.5 GJ 625 0.300 GJ 625 b 0.010 6.6 HD 219134 HD 219134 h 0.280 6.6 HD 219134 HD 219134 e 0.200 6.6 HD 219134 HD 219134 d 0.067 6.6 HD 219134 HD
    [Show full text]
  • 283 — 12 July 2016 Editor: Bo Reipurth ([email protected]) List of Contents
    THE STAR FORMATION NEWSLETTER An electronic publication dedicated to early stellar/planetary evolution and molecular clouds No. 283 — 12 July 2016 Editor: Bo Reipurth ([email protected]) List of Contents The Star Formation Newsletter Interview ...................................... 3 Perspective .................................... 5 Editor: Bo Reipurth [email protected] Abstracts of Newly Accepted Papers ........... 9 Technical Editor: Eli Bressert Abstracts of Newly Accepted Major Reviews . 33 [email protected] Dissertation Abstracts ........................ 34 Technical Assistant: Hsi-Wei Yen New Jobs ..................................... 35 [email protected] Meetings ..................................... 37 Editorial Board Summary of Upcoming Meetings ............. 37 Joao Alves Alan Boss Jerome Bouvier Lee Hartmann Thomas Henning Cover Picture Paul Ho Jes Jorgensen The image, obtained with the Hubble Space Tele- Charles J. Lada scope, shows photoevaporating globules embedded Thijs Kouwenhoven in the Carina Nebula. Michael R. Meyer Image courtesy NASA, ESA, N. Smith (University Ralph Pudritz of California, Berkeley), and The Hubble Heritage Luis Felipe Rodr´ıguez Team (STScI/AURA) Ewine van Dishoeck Hans Zinnecker The Star Formation Newsletter is a vehicle for fast distribution of information of interest for as- tronomers working on star and planet formation Submitting your abstracts and molecular clouds. You can submit material for the following sections: Abstracts of recently Latex macros for submitting abstracts
    [Show full text]
  • Arxiv:1810.09457V1
    Draft version October 24, 2018 Typeset using LATEX twocolumn style in AASTeX61 SCEXAO/CHARIS NEAR-INFRARED DIRECT IMAGING, SPECTROSCOPY, AND FORWARD-MODELING OF κ AND b: A LIKELY YOUNG, LOW-GRAVITY SUPERJOVIAN COMPANION Thayne Currie,1,2,3 Timothy D. Brandt,4 Taichi Uyama,5 Eric L. Nielsen,6 Sarah Blunt,7 Olivier Guyon,2,8,9,10 Motohide Tamura,5,10 Christian Marois,11,12 Kyle Mede,5 Masayuki Kuzuhara,10 Tyler D. Groff,13 Nemanja Jovanovic,14 N. Jeremy Kasdin,15 Julien Lozi,2 Klaus Hodapp,16 Jeffrey Chilcote,17 Joseph Carson,18 Frantz Martinache,19 Sean Goebel,16 Carol Grady,3,13 Michael McElwain,13 Eiji Akiyama,20 Ruben Asensio-Torres,21 Masa Hayashi,22 Markus Janson,21 Gillian R. Knapp,23 Jungmi Kwon,24 Jun Nishikawa,25 Daehyeon Oh,26 Joshua Schlieder,13 Eugene Serabyn,27 Michael Sitko,28 and Nour Skaf29 1NASA-Ames Research Center, Moffett Field, CA, USA 2Subaru Telescope, National Astronomical Observatory of Japan, 650 North A‘oho¯ku¯ Place, Hilo, HI 96720, USA 3Eureka Scientific, 2452 Delmer Street Suite 100, Oakland, CA, USA 4Department of Physics, University of California, Santa Barbara, Santa Barbara, California, USA 5Department of Astronomy, The University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan 6Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 7Department of Astronomy, Harvard University, 60 Garden St., Cambridge, Massachusetts, USA 8Steward Observatory, University of Arizona, Tucson, AZ 85721, USA 9College of Optical Sciences, University of Arizona, Tucson, AZ 85721, USA 10Astrobiology Center of NINS, 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan 11National Research Council of Canada Herzberg, 5071 West Saanich Rd, Victoria, BC, V9E 2E7, Canada 12University of Victoria, 3800 Finnerty Rd, Victoria, BC, V8P 5C2, Canada 13NASA-Goddard Space Flight Center, Greenbelt, MD, USA 14Department of Astronomy, California Institute of Technology, 1200 E.
    [Show full text]
  • Thirty Meter Telescope Detailed Science Case: 2015
    TMT.PSC.TEC.07.007.REL02 PAGE 1 DETAILEDThirty SCIENCE CASE: Meter 2015 TelescopeApril 29, 2015 Detailed Science Case: 2015 International Science Development Teams & TMT Science Advisory Committee TMT.PSC.TEC.07.007.REL02 PAGE I DETAILED SCIENCE CASE: 2015 April 29, 2015 Front cover: Shown is the Thirty Meter Telescope during nightime operations using the Laser Guide Star Facility (LGSF). The LGSF will create an asterism of stars, each asterism specifically chosen according to the particular adaptive optics system being used and the science program being conducted. TMT.PSC.TEC.07.007.REL02 PAGE II DETAILED SCIENCE CASE: 2015 April 29, 2015 DETAILED SCIENCE CASE: 2015 TMT.PSC.TEC.07.007.REL02 1 DATE: (April 29, 2015) Low resolution version Full resolution version available at: http://www.tmt.org/science-case © Copyright 2015 TMT Observatory Corporation arxiv.org granted perpetual, non-exclusive license to distribute this article 1 Minor revisions made 6/3/2015 to correct spelling, acknowledgements and references TMT.PSC.TEC.07.007.REL02 PAGE III DETAILED SCIENCE CASE: 2015 April 29, 2015 PREFACE For tens of thousands of years humans have looked upward and tried to find meaning in what they see in the sky, trying to understand the context in which they and their world exists. Consequently, astronomy is the oldest of the sciences. Since Aristotle began systematically recording the motions of the planets and formulating the first models of the universe there have been over 2350 years of scientific study of the sky. The earliest scientists explained their observations with the earth-centered universe model and little more than two millennia later we now live in an age where we are beginning to characterize exoplanets and systematically probing the evolution of the universe from its earliest moments to the present day.
    [Show full text]