Dr. Meredith A. Macgregor
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Interstellar Medium Sculpting of the HD 32297 Disk
DRAFT VERSION MAY 31, 2018 Preprint typeset using LATEX style emulateapj v. 7/15/03 INTERSTELLAR MEDIUM SCULPTING OF THE HD 32297 DEBRIS DISK JOHN H. DEBES1,2,ALYCIA J. WEINBERGER3, MARC J. KUCHNER1 Draft version May 31, 2018 ABSTRACT We detect the HD 32297 debris disk in scattered light at 1.6 and 2.05 µm. We use these new observations together with a previous scattered light image of the disk at 1.1 µm to examine the structure and scattering efficiency of the disk as a function of wavelength. In addition to surface brightness asymmetries and a warped morphology beyond ∼1.′′5 for one lobe of the disk, we find that there exists an asymmetry in the spectral features of the grains between the northeastern and southwestern lobes. The mostly neutral color of the disk lobes imply roughly 1 µm-sized grains are responsible for the scattering. We find that the asymmetries in color and morphology can plausibly be explained by HD 32297’s motion into a dense ISM cloud at a relative velocity of15kms−1. We modeltheinteractionofdustgrainswith HIgasin thecloud. We argue that supersonic ballistic drag can explain the morphology of the debris disks of HD 32297, HD 15115, and HD 61005. Subject headings: stars:individual(HD 32297)—stars:individual(HD 15115)—stars:individual(HD 61005)— circumstellar disks—methods:n-body simulations—ISM ′′ 1. INTRODUCTION distances >0. 75 the disk is brighter on the NE side, i.e. re- Debris disks are created by the outgassing and collisions of versed from the asymmetry seen in scattered light images planetesimals that may resemble analogues to the comets, as- (Moerchen et al. -
Astrophysics Division Astrophysics Douglas Hudgins Program Scientist, Exoplanet Exploration Program Key NASA/SMD Science Themes
National Aeronautics and Space Administration NASA and the Search for Life on Planets around Other Stars A presentation to the National Academies Committee on Exoplanet Science Strategy 6 March 2018 Paul Hertz Director, Astrophysics Division Astrophysics Douglas Hudgins Program Scientist, Exoplanet Exploration Program Key NASA/SMD Science Themes Protect and Improve Life on Earth Search for Life Elsewhere Discover the Secrets of the Universe 2 Talk summary 3 NASA’s Exoplanet Exploration Program Space Missions and Mission Studies Public Communications Kepler, WFIRST Decadal Studies K2 Starshade Coronagraph Supporting Research & Technology Key Sustaining Research NASA Exoplanet Science Institute Technology Development Coronagraph Masks Large Binocular Keck Single Aperture Telescope Interferometer Imaging and RV High-Contrast Deployable Archives, Tools, Sagan Fellowships, Imaging Starshades Professional Engagement NN-EXPLORE https://exoplanets.nasa.gov 4 Foundational Documents for the NASA’s Astrophysics Division 5 NASA’s cross-divisional Search for Life Elsewhere ASTROPHYSICS • Exoplanet detection and Planetary SCIENCE/ characterization ASTROBIOLOGY • Stellar characterization • Comparative planetology • Mission data analysis • Planetary atmospheres Hubble, Spitzer, Kepler, • Assessment of observable TESS, JWST, WFIRST, biosignatures etc. • Habitability EARTH SCIENCES • GCM • Planets as systems PLANETARY SCIENCE RESEARCH HELIOPHYSICS • Exoplanet characterization • Stellar characterization • Protoplanetary disks • Stellar winds • Planet formation • Detection of planetary • Comparative planetology magnetospheres 6 Exoplanet Exploration at NASA 2007 - present 7 The Spitzer Space Telescope For the last decade, the Spitzer Space Telescope has used both spectroscopic and photometric measurements in the mid-IR to probe exoplanets and exoplanetary systems. • Spitzer follow up observations of known transiting systems have revealed additional, new planets and helped refine measurements of the size and orbital dynamics of known planets as small as the Earth. -
Arxiv:1811.01508V1 [Astro-Ph.SR] 5 Nov 2018 the Nearby, Young, Argus Association: Membership, Age, and Dusty Debris Disks 2
The Nearby, Young, Argus Association: Membership, Age, and Dusty Debris Disks B. Zuckerman1 1Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA E-mail: [email protected] Abstract. The reality of a field Argus Association has been doubted in some papers in the literature. We apply Gaia DR2 data to stars previously suggested to be Argus members and conclude that a true association exists with age 40-50 Myr and containing many stars within 100 pc of Earth; β Leo and 49 Cet are two especially interesting members. Based on youth and proximity to Earth, Argus is one of the better nearby moving groups to target in direct imaging programs for dusty debris disks and young planets. PACS numbers: 97.10.Tk arXiv:1811.01508v1 [astro-ph.SR] 5 Nov 2018 The Nearby, Young, Argus Association: Membership, Age, and Dusty Debris Disks 2 1. Introduction The solar vicinity is blessed with an assortment of youthful stars with ages that span the range 10 to 200 Myr. Within 100 pc of Earth a dozen or so coeval, co-moving groups were identified (Mamajek 2016) prior to the release of the Gaia DR2 catalog (Gaia Colaboration et al 2018; Lindegren et al 2018). Many nearby stars exist that appear to be youthful but have not been placed into any of these groups. With the help of Gaia, new kinematic groups can be identified. As recently as 20 years ago only a handful of youthful stars with reasonably reliable ages were known within 100 pc of Earth. With Gaia and appropriate follow-up observations, it now appears likely that a few 1000 will ultimately be identified. -
Discovery of Extreme Asymmetry in the Debris Disk Surrounding HD 15115
Submitted to ApJ Letters December 18, 2006; Accepted April 04, 2007 A Preprint typeset using LTEX style emulateapj v. 08/22/09 DISCOVERY OF EXTREME ASYMMETRY IN THE DEBRIS DISK SURROUNDING HD 15115 Paul Kalas1,2, Michael P. Fitzgerald1,2, James R. Graham1,2 Submitted to ApJ Letters December 18, 2006; Accepted April 04, 2007 ABSTRACT We report the first scattered light detection of a dusty debris disk surrounding the F2V star HD 15115 using the Hubble Space Telescope in the optical, and Keck adaptive optics in the near-infrared. The most remarkable property of the HD 15115 disk relative to other debris disks is its extreme length asymmetry. The east side of the disk is detected to ∼315 AU radius, whereas the west side of the disk has radius >550 AU. We find a blue optical to near-infrared scattered light color relative to the star that indicates grain scattering properties similar to the AU Mic debris disk. The existence of a large debris disk surrounding HD 15115 adds further evidence for membership in the β Pic moving group, which was previously argued based on kinematics alone. Here we hypothesize that the extreme disk asymmetry is due to dynamical perturbations from HIP 12545, an M star 0.5◦ (0.38 pc) east of HD 15115 that shares a common proper motion vector, heliocentric distance, galactic space velocity, and age. Subject headings: stars: individual(HD 15115) - circumstellar matter 1. INTRODUCTION is consistent with a single temperature dust belt at ∼35 Volume-limited, far-infrared surveys of the solar neigh- AU radius with an estimated dust mass of 0.047 M⊕ borhood suggest that ∼15% of main sequence stars have (Zuckerman & Song 2004; Williams & Andrews 2006). -
Theory of Debris Disks Modeling
THEORY OF DEBRIS DISKS MODELING Jean-Charles Augereau, IPAG – Grenoble, France 2 What is a debris disk? Star Fomalhaut : composite HST+ALMA image Kalas et al. 2005, Boley et al. 2012 • Extrasolar planetary systems have planets, but also comets and asteroids ! • Extrasolar comets/asteroids manifest themselves when they release dust : collisions, evaporation ! • Debris disks • cold (~20-100K), extra-solar analogs to the Kuiper Belt • warm/hot (up to ~1500/2000K), extra-solar analogs to the asteroid belt and zodiacal dust 3 Why modeling debris disks? What do we want to know? • Grain properties: • Spatial distribution: • composition of • interaction with the unseen planets population of • history of the planetesimals formation and • size distribution evolution of planetesimals Toward a complete census of the constituents of extrasolar planetary systems, and a detailed understanding of their overall dynamics. 4 Theory of debris disk modeling Spectral Energy Distributions. Blackbody fitting, and limitations 10.0 1.0 Flux in Jy 0.1 • Hundreds of debris disks detected • Only ~40-50 have been spatially 1 10 100 1000 resolved [µm] 5 • Fractional luminosity: Spectral energy f = LIR / Lstar distribution ! ! 10.0 ! ! 1.0 !Flux in Jy Lstar ! 0.1 LIR ! 1 10 100 1000 ! [µm] • f ~ optical thickness ≪ 1 u the disk is optically thin In this example: f = 3x10-4 6 • Fit of a blackbody to the disk emission Spectral energy u disk mean temperature Tdust distribution ! • Spherical blackbody grains in thermal equilibrium: Tdust u disk radius Labsorbed = Lemitted -
A Near-Infrared Interferometric Survey of Debris-Disk Stars: VII
A near-infrared interferometric survey of debris- disk stars: VII. The hot-to-warm dust connection Item Type Article; text Authors Absil, O.; Marion, L.; Ertel, S.; Defrère, D.; Kennedy, G.M.; Romagnolo, A.; Le Bouquin, J.-B.; Christiaens, V.; Milli, J.; Bonsor, A.; Olofsson, J.; Su, K.Y.L.; Augereau, J.-C. Citation Absil, O., Marion, L., Ertel, S., Defrère, D., Kennedy, G. M., Romagnolo, A., Le Bouquin, J.-B., Christiaens, V., Milli, J., Bonsor, A., Olofsson, J., Su, K. Y. L., & Augereau, J.-C. (2021). A near-infrared interferometric survey of debris-disk stars: VII. The hot-to-warm dust connection. Astronomy and Astrophysics, 651. DOI 10.1051/0004-6361/202140561 Publisher EDP Sciences Journal Astronomy and Astrophysics Rights Copyright © ESO 2021. Download date 05/10/2021 23:39:44 Item License http://rightsstatements.org/vocab/InC/1.0/ Version Final published version Link to Item http://hdl.handle.net/10150/661189 A&A 651, A45 (2021) Astronomy https://doi.org/10.1051/0004-6361/202140561 & © ESO 2021 Astrophysics A near-infrared interferometric survey of debris-disk stars VII. The hot-to-warm dust connection? O. Absil1,?? , L. Marion1, S. Ertel2,3 , D. Defrère4 , G. M. Kennedy5, A. Romagnolo6, J.-B. Le Bouquin7, V. Christiaens8 , J. Milli7 , A. Bonsor9 , J. Olofsson10,11 , K. Y. L. Su3 , and J.-C. Augereau7 1 STAR Institute, Université de Liège, 19c Allée du Six Août, 4000 Liège, Belgium e-mail: [email protected] 2 Large Binocular Telescope Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA 3 Steward Observatory, Department of Astronomy, University of Arizona, 993 N. -
Disks in Nearby Planetary Systems with JWST and ALMA
Disks in Nearby Planetary Systems with JWST and ALMA Meredith A. MacGregor NSF Postdoctoral Fellow Carnegie Department of Terrestrial Magnetism 233rd AAS Meeting ExoPAG 19 January 6, 2019 MacGregor Circumstellar Disk Evolution molecular cloud 0 Myr main sequence star + planets (?) + debris disk (?) Star Formation > 10 Myr pre-main sequence star + protoplanetary disk Planet Formation 1-10 Myr MacGregor Debris Disks: Observables First extrasolar debris disk detected as “excess” infrared emission by IRAS (Aumann et al. 1984) SPHERE/VLT Herschel ALMA VLA Boccaletti et al (2015), Matthews et al. (2015), MacGregor et al. (2013), MacGregor et al. (2016a) Now, resolved at wavelengthsfrom from Herschel optical DUNES (scattered light) to millimeter and radio (thermal emission) MacGregor Planet-Disk Interactions Planets orbiting a star can gravitationally perturb an outer debris disk Expect to see a variety of structures: warps, clumps, eccentricities, central offsets, sharp edges, etc. Goal: Probe for wide separation planets using debris disk structure HD 15115 β Pictoris Kuiper Belt Asymmetry Warp Resonance Kalas et al. (2007) Lagrange et al. (2010) Jewitt et al. (2009) MacGregor Debris Disks Before ALMA Epsilon Eridani HD 95086 Tau Ceti Beta PictorisHR 4796A HD 107146 AU Mic Greaves+ (2014) Su+ (2015) Lawler+ (2014) Vandenbussche+ (2010) Koerner+ (1998) Hughes+ (2011) Matthews+ (2015) 49 Ceti HD 181327 HD 21997 Fomalhaut HD 10647 (q1 Eri) Eta Corvi HR 8799 Roberge+ (2013) Lebreton+ (2012) Moor+ (2015) Acke+ (2012) Liseau+ (2010) Lebreton+ (2016) -
Redox DAS Artist List for Period: 01.10.2017
Page: 1 Redox D.A.S. Artist List for period: 01.10.2017 - 31.10.2017 Date time: Number: Title: Artist: Publisher Lang: 01.10.2017 00:02:40 HD 60753 TWO GHOSTS HARRY STYLES ANG 01.10.2017 00:06:22 HD 05631 BANKS OF THE OHIO OLIVIA NEWTON JOHN ANG 01.10.2017 00:09:34 HD 60294 BITE MY TONGUE THE BEACH ANG 01.10.2017 00:13:16 HD 26897 BORN TO RUN SUZY QUATRO ANG 01.10.2017 00:18:12 HD 56309 CIAO CIAO KATARINA MALA SLO 01.10.2017 00:20:55 HD 34821 OCEAN DRIVE LIGHTHOUSE FAMILY ANG 01.10.2017 00:24:41 HD 08562 NISEM JAZ SLAVKO IVANCIC SLO 01.10.2017 00:28:29 HD 59945 LEPE BESEDE PROTEUS SLO 01.10.2017 00:31:20 HD 03206 BLAME IT ON THE WEATHERMAN B WITCHED ANG 01.10.2017 00:34:52 HD 16013 OD TU NAPREJ NAVDIH TABU SLO 01.10.2017 00:38:14 HD 06982 I´M EVERY WOMAN WHITNEY HOUSTON ANG 01.10.2017 00:43:05 HD 05890 CRAZY LITTLE THING CALLED LOVE QUEEN ANG 01.10.2017 00:45:37 HD 57523 WHEN I WAS A BOY JEFF LYNNE (ELO) ANG 01.10.2017 00:48:46 HD 60269 MESTO (FEAT. VESNA ZORNIK) BREST SLO 01.10.2017 00:52:21 HD 06008 DEEPLY DIPPY RIGHT SAID FRED ANG 01.10.2017 00:55:35 HD 06012 UNCHAINED MELODY RIGHTEOUS BROTHERS ANG 01.10.2017 00:59:10 HD 60959 OKNA ORLEK SLO 01.10.2017 01:03:56 HD 59941 SAY SOMETHING LOVING THE XX ANG 01.10.2017 01:07:51 HD 15174 REAL GOOD LOOKING BOY THE WHO ANG 01.10.2017 01:13:37 HD 59654 RECI MI DA MANOUCHE SLO 01.10.2017 01:16:47 HD 60502 SE PREPOZNAS SHEBY SLO 01.10.2017 01:20:35 HD 06413 MARGUERITA TIME STATUS QUO ANG 01.10.2017 01:23:52 HD 06388 MAMA SPICE GIRLS ANG 01.10.2017 01:27:25 HD 02680 HIGHER GROUND ERIC CLAPTON ANG 01.10.2017 01:31:20 HD 59929 NE POZABI, DA SI LEPA LUKA SESEK & PROPER SLO 01.10.2017 01:34:57 HD 02131 BONNIE & CLYDE JAY-Z FEAT. -
Abstracts for “Extreme Solar Systems”
Abstracts for \Extreme Solar Systems" Talk Abstracts \Pulsar Planets" Wolszczan, A. I will review the history and current status of our understanding of the PSR B1257+12 planetary system. I will also discuss neutron star planet formation scenarios and their relevance to formation and evolution of planetary systems around other stars. 1 \Extrasolar Planets: The Golden Age of Radial Velocities" Udry, S. Twelve years after the discovery of 51Pegb more than 220 planets have been detected with the radial-velocity technique. The information gathered on the orbital-element distributions, as well as on the characteristics of the planet-host stars, have largely contributed to improve our understanding of planet formation. In this presentation I will review these results with a special focus on the recent efforts of the past few years to improve the parameter space of stellar and planetary properties. The complementary and fundamental role of radial velocities in the planetary transit cases and the additional information they bring on the planet structure and on the geometry of the systems will be discussed as well. 2 \From Hot Jupiters to Hot Super-Earths" Mayor, M. In the last twelve years, more than 200 exoplanets have been detected. These discoveries have revealed the impressive diversity of exoplanet orbital properties. The past twelve years have also witnessed a remarkable improvement of the precision of radial velocity measurements with a gain of about a factor 100. Thanks to the HARPS spectro- graph installed in 2003 at la Silla Observatory ,numerous planets with masses as small as a few earth-masses have been detected. -
Planet Formation in Dense Star Clusters
Planet Formation in Dense Star Clusters Henry Throop Department of Space Studies Southwest Research Institute (SwRI), Boulder, Colorado Collaborators: John Bally (U. Colorado) Nickolas Moeckel (Cambridge) Universidad de Guanajuato 23 de octubre 2009 HBT 28-Jun-2005 3 Orion Constellation (visible light) Orion constellation H-alpha Orion constellation H-alpha Orion Molecular Clouds >105 Msol 100 pc long Orion core (visible light) Orion core (visible light) Orion Star Forming Region • Closest bright star-forming region to Earth • Distance ~ 1500 ly • Age ~ 10 Myr • Radius ~ few ly • Mean separation ~ 104 AU Orion Trapezium cluster Massive stars Low mass stars; Disks with tails • LargestLargest Orion Orion disk: disk: 114-426, 114-426, D ~ 1200 diameterAU 1200 AU • Dust grains in disk are grey, and do not redden light as they extinct it • Dust grains have grown to a few microns or greater in < 1 Myr Star Formation 1961 view: “Whether we've ever seen a star form or not is still debated. The next slide is the one piece of evidence that suggests that we have. Here's a picture taken in 1947 of a region of gas, with some stars in it. And here's, only two years later, we see two new bright spots. The idea is that what happened is that gravity has...” Richard Feynman, Lectures on Physics HBT 1628-Jun-2005 Star Formation 1961 view: “Whether we've ever seen a star form or not is still debated. The next slide is the one piece of evidence that suggests that we have. Here's a picture taken in 1947 of a region of gas, with some stars in it. -
A PLANET-SCULPTING SCENARIO for the HD 61005 DEBRIS DISK
UCLA UCLA Previously Published Works Title BRINGING "tHE MOTH" to LIGHT: A PLANET-SCULPTING SCENARIO for the HD 61005 DEBRIS DISK Permalink https://escholarship.org/uc/item/1h77k16g Journal Astronomical Journal, 152(4) ISSN 0004-6256 Authors Esposito, TM Fitzgerald, MP Graham, JR et al. Publication Date 2016-10-01 DOI 10.3847/0004-6256/152/4/85 Peer reviewed eScholarship.org Powered by the California Digital Library University of California The Astronomical Journal, 152:85 (16pp), 2016 October doi:10.3847/0004-6256/152/4/85 © 2016. The American Astronomical Society. All rights reserved. BRINGING “THE MOTH” TO LIGHT: A PLANET-SCULPTING SCENARIO FOR THE HD 61005 DEBRIS DISK Thomas M. Esposito1,2, Michael P. Fitzgerald1, James R. Graham2, Paul Kalas2,3, Eve J. Lee2, Eugene Chiang2, Gaspard Duchêne2,4, Jason Wang2, Maxwell A. Millar-Blanchaer5,6, Eric Nielsen3,7, S. Mark Ammons8, Sebastian Bruzzone9, Robert J. De Rosa2, Zachary H. Draper10,11, Bruce Macintosh7, Franck Marchis3, Stanimir A. Metchev9,12, Marshall Perrin13, Laurent Pueyo13, Abhijith Rajan14, Fredrik T. Rantakyrö15, David Vega3, and Schuyler Wolff16 1 Department of Physics and Astronomy, 430 Portola Plaza, University of California, Los Angeles, CA 90095-1547, USA; [email protected] 2 Department of Astronomy, University of California, Berkeley, CA 94720, USA 3 SETI Institute, Carl Sagan Center, 189 Bernardo Avenue, Mountain View, CA 94043, USA 4 Université Grenoble Alpes/CNRS, Institut de Planétologie et d’Astrophysique de Grenoble, F-38000 Grenoble, France 5 Department of -
Dissecting the Moth: Discovery of an Off-Centered Ring in the HD 61005
Astronomy & Astrophysics manuscript no. moth˙ebuenzli c ESO 2018 August 15, 2018 Letter to the Editor Dissecting the Moth: Discovery of an off-centered ring in the HD 61005 debris disk with high-resolution imaging⋆ E. Buenzli1, C. Thalmann2, A. Vigan3, A. Boccaletti4, G. Chauvin5, J.C. Augereau5, M.R. Meyer1, F. M´enard5, S. Desidera6, S. Messina7, T. Henning2, J. Carson8,2, G. Montagnier9, J.L. Beuzit5, M. Bonavita10, A. Eggenberger5, A.M. Lagrange5, D. Mesa6, D. Mouillet5, and S. P. Quanz1 1 Institute for Astronomy, ETH Zurich, 8093 Zurich, Switzerland e-mail: [email protected] 2 Max Planck Institute for Astronomy, Heidelberg, Germany 3 Laboratoire d’Astrophysique de Marseille, UMR 6110, CNRS, Universit´ede Provence, 13388 Marseille, France 4 LESIA, Observatoire de Paris-Meudon, 92195 Meudon, France 5 Laboratoire d’Astrophysique de Grenoble, UMR 5571, CNRS, Universit´eJoseph Fourier, 38041 Grenoble, France 6 INAF - Osservatorio Astronomico di Padova, Padova, Italy 7 INAF - Osservatorio Astrofisico di Catania, Italy 8 College of Charleston, Department of Physics & Astronomy, Charleston, South Carolina, USA 9 European Southern Observatory: Casilla 19001, Santiago 19, Chile 10 University of Toronto, Toronto, Canada received 22 September 2010 / accepted 09 November 2010 ABSTRACT The debris disk known as “The Moth” is named after its unusually asymmetric surface brightness distribution. It is located around the ∼90 Myr old G8V star HD 61005 at 34.5 pc and has previously been imaged by the HST at 1.1 and 0.6 µm. Polarimetric observations suggested that the circumstellar material consists of two distinct components, a nearly edge-on disk or ring, and a swept-back feature, the result of interaction with the interstellar medium.