The Exoplanet Revolution
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Arxiv:1910.11169V1 [Astro-Ph.EP] 24 Oct 2019 Metchev Et Al.(2004) Due to the Detection of a Strong Mid- Tinuum and at HCO+ and CO Gas Emission Lines
Astronomy & Astrophysics manuscript no. PDS70_v2 c ESO 2019 October 25, 2019 VLT/SPHERE exploration of the young multiplanetary system PDS70? D. Mesa1, M. Keppler2, F. Cantalloube2, L. Rodet3, B. Charnay4, R. Gratton1, M. Langlois5; 6, A. Boccaletti4, M. Bonnefoy3, A. Vigan6, O. Flasseur7, J. Bae8, M. Benisty3; 9, G. Chauvin3; 9, J. de Boer10, S. Desidera1, T. Henning2, A.-M. Lagrange3, M. Meyer11, J. Milli12, A. Müller2, B. Pairet13, A. Zurlo14; 15; 6, S. Antoniucci16, J.-L. Baudino17, S. Brown Sevilla2, E. Cascone18, A. Cheetham19, R.U. Claudi1, P. Delorme3, V. D’Orazi1, M. Feldt2, J. Hagelberg19, M. Janson20, Q. Kral4, E. Lagadec21, C. Lazzoni1, R. Ligi22, A.-L. Maire2; 23, P. Martinez21, F. Menard3, N. Meunier3, C. Perrot4; 24; 25, S. Petrus3, C. Pinte26; 3, E.L. Rickman19, S. Rochat3, D. Rouan4, M. Samland2; 20, J.-F. Sauvage27; 6, T. Schmidt4; 28, S. Udry19, L. Weber19, F. Wildi19 (Affiliations can be found after the references) Received / accepted ABSTRACT Context. PDS 70 is a young (5.4 Myr), nearby (∼113 pc) star hosting a known transition disk with a large gap. Recent observations with SPHERE and NACO in the near-infrared (NIR) allowed us to detect a planetary mass companion, PDS 70 b, within the disk cavity. Moreover, observations in Hα with MagAO and MUSE revealed emission associated to PDS 70 b and to another new companion candidate, PDS 70 c, at a larger separation from the star. PDS 70 is the only multiple planetary system at its formation stage detected so far through direct imaging. Aims. Our aim is to confirm the discovery of the second planet PDS 70 c using SPHERE at VLT, to further characterize its physical properties, and search for additional point sources in this young planetary system. -
Ann Merchant Boesgaard Publications Merchant, A. E., Bodenheimer, P., and Wallerstein, G
Ann Merchant Boesgaard Publications Merchant, A. E., Bodenheimer, P., and Wallerstein, G. (1965). “The Lithium Isotope Ratio in Two Hyades F Stars.” Ap. J., 142, 790. Merchant, A. E. (1966). “Beryllium in F- and G-Type Dwarfs.” Ap. J., 143, 336. Hodge, P. W., and Merchant, A. E. (1966). “Photometry of SO Galaxies II. The Peculiar Galaxy NGC 128.” Ap. J., 144, 875. Merchant, A. E. (1967). “The Abundance of Lithium in Early M-Type Stars.” Ap. J., 147, 587. Merchant, A. E. (1967). “Measured Equivalent Widths in Early M-Type Stars.” Lick Obs. Bull. No. 595 (Univ. of California Press). Boesgaard, A. M. (1968). “Isotopes of Magnesium in Stellar Atmosphere.” Ap. J., 154, 185. Boesgaard, A. M. (1968). “Observations of Beryllium in Stars.” Highlights of Astron- omy, ed. L. Perek (Dordrecht: D. Reidel), p. 237. Boesgaard, A. M. (1969). “Intensity Variation in Ca Emission in an MS Star.” Pub. A. S. P., 81, 283. Boesgaard, A. M. (1969). “Observational Clues to the Evolution of M Giant Stars.” Pub. A. S. P., 81, 365. Boesgaard, A. M. (1970). “The Lithium Isotope Ratio in δ Sagittae.” Ap. J., 159, 727. Boesgaard, A. M. (1970). “The Ratio of Titanium to Zirconium in Late-Type Stars.” Ap. J., 161, 163. Boesgaard, A. M. (1970). “On the Lithium Content in Late-Type Giants.” Ap. Letters, 5, 145. Boesgaard, A. M. (1970). “Lithium in Heavy-Metal Red Giants.” Ap. J., 161, 1003. Boesgaard, A. M. (1971). “The Lithium Content of Capella.” Ap. J., 167, 511. Boesgaard, A. M. (1973). “Iron Emission Lines in a Orionis.” In Stellar Chromospheres, eds. -
Urania Nr 3/2005
> /2005 (717) urania 3/tom LXXVI maj—czerwiec mhćirn iVlich jp f f l owiek, który świat nauczył rnier> życe(?) wokóf planetoid Fotome anzytów za pomocą rnaiych Europejskie Obserwatorium Południowe leskopami pomocniczymi (AT) o średnicy a dalej ogromne budynki mieszczące wiel (ESO) zbudowało w latach 1988-2002, na 1,8 m, które mogą zajmować 30 różnych kie teleskopy i 2 kopuły teleskopów pomoc ściętym wierzchołku góry Cerro Paranal pozycji, będą stanowiły ciągle rozbudowy niczych (obecnie są 2 AT, będzie ich 8). (2635 m n.p.m.) na pustyni Atacama w Chi wany instrument interferometryczny (VLTI) Na górnym zdjęciu widzimy teleskop „z gó le, Bardzo Duży Teleskop (VLT). Składa o bazie sięgającej przeszło 200 m, które ry" wraz z okolicznym krajobrazem, toro się on z czterech teleskopów o średnicy go rozdzielczość (0,001 sekundy łuku) bę wiskami teleskopów AT i drogami kanałów 8,2 m, mogących kierować zebrane świa dzie tak wielka, że można by widzieć nim optycznych prowadzących zebrane świa tło do wspólnego ogniska. Razem zbierają astronautę na Księżycu. Dolne zdjęcie tło do wspólnego ogniska interferometru one tyle światła, ile zbierałby teleskop przedstawia ogólny, obecny (2005 r.) wi oznaczonego gwiazdką. Idea i zasady o średnicy 16 m, a pracując w systemie dok tego obserwatorium. Na pierwszym działania tego instrumentu wywodzą się interferometrycznym, stanowią teleskop planie widzimy torowisko i stanowiska ob z odkryć i prac Alberta Michelsona. o średnicy prawie 130 m. Wspomagane te serwacyjne dla teleskopów pomocniczych, Zdjęcia ESO U R A N IA - POSTtPY ASTRONOMII 3/2005 Szanowni i Drodzy Czytelnicy, Interferometria, jako technika badawcza, zdobywa coraz szersze pola zastosowań w astronomii. -
The Nearest Stars: a Guided Tour by Sherwood Harrington, Astronomical Society of the Pacific
www.astrosociety.org/uitc No. 5 - Spring 1986 © 1986, Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, CA 94112. The Nearest Stars: A Guided Tour by Sherwood Harrington, Astronomical Society of the Pacific A tour through our stellar neighborhood As evening twilight fades during April and early May, a brilliant, blue-white star can be seen low in the sky toward the southwest. That star is called Sirius, and it is the brightest star in Earth's nighttime sky. Sirius looks so bright in part because it is a relatively powerful light producer; if our Sun were suddenly replaced by Sirius, our daylight on Earth would be more than 20 times as bright as it is now! But the other reason Sirius is so brilliant in our nighttime sky is that it is so close; Sirius is the nearest neighbor star to the Sun that can be seen with the unaided eye from the Northern Hemisphere. "Close'' in the interstellar realm, though, is a very relative term. If you were to model the Sun as a basketball, then our planet Earth would be about the size of an apple seed 30 yards away from it — and even the nearest other star (alpha Centauri, visible from the Southern Hemisphere) would be 6,000 miles away. Distances among the stars are so large that it is helpful to express them using the light-year — the distance light travels in one year — as a measuring unit. In this way of expressing distances, alpha Centauri is about four light-years away, and Sirius is about eight and a half light- years distant. -
Arxiv:1809.07342V1 [Astro-Ph.SR] 19 Sep 2018
Draft version September 21, 2018 Preprint typeset using LATEX style emulateapj v. 11/10/09 FAR-ULTRAVIOLET ACTIVITY LEVELS OF F, G, K, AND M DWARF EXOPLANET HOST STARS* Kevin France1, Nicole Arulanantham1, Luca Fossati2, Antonino F. Lanza3, R. O. Parke Loyd4, Seth Redfield5, P. Christian Schneider6 Draft version September 21, 2018 ABSTRACT We present a survey of far-ultraviolet (FUV; 1150 { 1450 A)˚ emission line spectra from 71 planet- hosting and 33 non-planet-hosting F, G, K, and M dwarfs with the goals of characterizing their range of FUV activity levels, calibrating the FUV activity level to the 90 { 360 A˚ extreme-ultraviolet (EUV) stellar flux, and investigating the potential for FUV emission lines to probe star-planet interactions (SPIs). We build this emission line sample from a combination of new and archival observations with the Hubble Space Telescope-COS and -STIS instruments, targeting the chromospheric and transition region emission lines of Si III,N V,C II, and Si IV. We find that the exoplanet host stars, on average, display factors of 5 { 10 lower UV activity levels compared with the non-planet hosting sample; this is explained by a combination of observational and astrophysical biases in the selection of stars for radial-velocity planet searches. We demonstrate that UV activity-rotation relation in the full F { M star sample is characterized by a power-law decline (with index α ≈ −1.1), starting at rotation periods & 3.5 days. Using N V or Si IV spectra and a knowledge of the star's bolometric flux, we present a new analytic relationship to estimate the intrinsic stellar EUV irradiance in the 90 { 360 A˚ band with an accuracy of roughly a factor of ≈ 2. -
Materials Challenges for the Starshot Lightsail
PERSPECTIVE https://doi.org/10.1038/s41563-018-0075-8 Materials challenges for the Starshot lightsail Harry A. Atwater 1*, Artur R. Davoyan1, Ognjen Ilic1, Deep Jariwala1, Michelle C. Sherrott 1, Cora M. Went2, William S. Whitney2 and Joeson Wong 1 The Starshot Breakthrough Initiative established in 2016 sets an audacious goal of sending a spacecraft beyond our Solar System to a neighbouring star within the next half-century. Its vision for an ultralight spacecraft that can be accelerated by laser radiation pressure from an Earth-based source to ~20% of the speed of light demands the use of materials with extreme properties. Here we examine stringent criteria for the lightsail design and discuss fundamental materials challenges. We pre- dict that major research advances in photonic design and materials science will enable us to define the pathways needed to realize laser-driven lightsails. he Starshot Breakthrough Initiative has challenged a broad nanocraft, we reveal a balance between the high reflectivity of the and interdisciplinary community of scientists and engineers sail, required for efficient photon momentum transfer; large band- Tto design an ultralight spacecraft or ‘nanocraft’ that can reach width, accounting for the Doppler shift; and the low mass necessary Proxima Centauri b — an exoplanet within the habitable zone of for the spacecraft to accelerate to near-relativistic speeds. We show Proxima Centauri and 4.2 light years away from Earth — in approxi- that nanophotonic structures may be well-suited to meeting such mately -
The Search for Another Earth – Part II
GENERAL ARTICLE The Search for Another Earth – Part II Sujan Sengupta In the first part, we discussed the various methods for the detection of planets outside the solar system known as the exoplanets. In this part, we will describe various kinds of exoplanets. The habitable planets discovered so far and the present status of our search for a habitable planet similar to the Earth will also be discussed. Sujan Sengupta is an 1. Introduction astrophysicist at Indian Institute of Astrophysics, Bengaluru. He works on the The first confirmed exoplanet around a solar type of star, 51 Pe- detection, characterisation 1 gasi b was discovered in 1995 using the radial velocity method. and habitability of extra-solar Subsequently, a large number of exoplanets were discovered by planets and extra-solar this method, and a few were discovered using transit and gravi- moons. tational lensing methods. Ground-based telescopes were used for these discoveries and the search region was confined to about 300 light-years from the Earth. On December 27, 2006, the European Space Agency launched 1The movement of the star a space telescope called CoRoT (Convection, Rotation and plan- towards the observer due to etary Transits) and on March 6, 2009, NASA launched another the gravitational effect of the space telescope called Kepler2 to hunt for exoplanets. Conse- planet. See Sujan Sengupta, The Search for Another Earth, quently, the search extended to about 3000 light-years. Both Resonance, Vol.21, No.7, these telescopes used the transit method in order to detect exo- pp.641–652, 2016. planets. Although Kepler’s field of view was only 105 square de- grees along the Cygnus arm of the Milky Way Galaxy, it detected a whooping 2326 exoplanets out of a total 3493 discovered till 2Kepler Telescope has a pri- date. -
ISPY-NACO Imaging Survey for Planets Around Young Stars Survey Description and Results from the first 2.5 Years of Observations? R
A&A 635, A162 (2020) Astronomy https://doi.org/10.1051/0004-6361/201937000 & © R. Launhardt et al. 2020 Astrophysics ISPY-NACO Imaging Survey for Planets around Young stars Survey description and results from the first 2.5 years of observations? R. Launhardt1, Th. Henning1, A. Quirrenbach2, D. Ségransan3, H. Avenhaus4,1, R. van Boekel1, S. S. Brems2, A. C. Cheetham1,3, G. Cugno4, J. Girard5, N. Godoy8,11, G. M. Kennedy6, A.-L. Maire1,10, S. Metchev7, A. Müller1, A. Musso Barcucci1, J. Olofsson8,11, F. Pepe3, S. P. Quanz4, D. Queloz9, S. Reffert2, E. L. Rickman3, H. L. Ruh2, and M. Samland1,12 1 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected] 2 Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany 3 Observatoire Astronomique de l’Université de Genève, 51 Ch. des Maillettes, 1290 Versoix, Switzerland 4 ETH Zürich, Institute for Particle Physics and Astrophysics, Wolfgang-Pauli-Str. 27, 8093 Zürich, Switzerland 5 Space Telescope Science Institute, Baltimore 21218, MD, USA 6 Department of Physics & Centre for Exoplanets and Habitability, University of Warwick, Coventry, UK 7 The University of Western Ontario, Department of Physics and Astronomy, 1151 Richmond Avenue, London, ON N6A 3K7, Canada 8 Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, Playa Ancha, Valparaíso, Chile 9 Cavendish Laboratory, J J Thomson Avenue, Cambridge, CB3 0HE, UK 10 STAR Institute, University of Liège, Allée du Six Août 19c, 4000 Liège, Belgium 11 Núcleo Milenio Formación Planetaria – NPF, Universidad de Valparaíso, Av. -
Annual Report 2016–2017 AAVSO
AAVSO The American Association of Variable Star Observers Annual Report 2016–2017 AAVSO Annual Report 2012 –2013 The American Association of Variable Star Observers AAVSO Annual Report 2016–2017 The American Association of Variable Star Observers 49 Bay State Road Cambridge, MA 02138-1203 USA Telephone: 617-354-0484 Fax: 617-354-0665 email: [email protected] website: https://www.aavso.org Annual Report Website: https://www.aavso.org/annual-report On the cover... At the 2017 AAVSO Annual Meeting.(clockwise from upper left) Knicole Colon, Koji Mukai, Dennis Conti, Kristine Larsen, Joey Rodriguez; Rachid El Hamri, Andy Block, Jane Glanzer, Erin Aadland, Jamin Welch, Stella Kafka; and (clockwise from upper left) Joey Rodriguez, Knicole Colon, Koji Mukai, Frans-Josef “Josch” Hambsch, Chandler Barnes. Picture credits In additon to images from the AAVSO and its archives, the editors gratefully acknowledge the following for their image contributions: Glenn Chaple, Shawn Dvorak, Mary Glennon, Bill Goff, Barbara Harris, Mario Motta, NASA, Gary Poyner, Msgr. Ronald Royer, the Mary Lea Shane Archives of the Lick Observatory, Chris Stephan, and Wheatley, et al. 2003, MNRAS, 345, 49. Table of Contents 1. About the AAVSO Vision and Mission Statement 1 About the AAVSO 1 What We Do 2 What Are Variable Stars? 3 Why Observe Variable Stars? 3 The AAVSO International Database 4 Observing Variable Stars 6 Services to Astronomy 7 Education and Outreach 9 2. The Year in Review Introduction 11 The 106th AAVSO Spring Membership Meeting, Ontario, California 11 The -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
1903Apj 18. .3415 the SPECTRUM of O CETL' by Joel Stebbins. On
.3415 18. 1903ApJ THE SPECTRUM OF o CETL' By Joel Stebbins. On account of the great instrumental power required for the observation of the spectra of faint objects, changes in the spectra of long-period variable stars have not been well studied. In fact, there is no star which undergoes a large variation in bright- ness whose spectrum has been systematically followed from maxi- mum to minimum, or vice versa. It is proposed to give here the results of a study of the spectrum of o Ceti> or Mira, made, at the suggestion of Director Campbell, with the thirty-six-inch refractor of the Lick Observatory, from June 1902 to January 1903. During this period the star faded in brightness from 3.8 to 9.0 magnitude. The first photograph of the spectrum was obtained about three weeks after the predicted time of maximum, and a series of plates was secured covering the interval to mini- mum. No negatives were obtained after the star had again begun to increase in brightness. The most important articles concerning the spectrum of Mira are those of Vogel,2 Sidgreaves,3 and Campbell.4 Neither Vogel nor Sidgreaves followed the star long enough to find much change in its spectrum, and Campbell’s work was mainly in con- nection with observations of the star for radial velocity, with the Mills spectrograph. INSTRUMENTS AND METHODS. The spectrograph used in my observations was the one employed rby Messrs. Campbell and Wright in their work on 1 “ Dissertation in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in the University of California,” Lick Observatory Bulletin No. -
Stellar Distances Teacher Guide
Stars and Planets 1 TEACHER GUIDE Stellar Distances Our Star, the Sun In this Exploration, find out: ! How do the distances of stars compare to our scale model solar system?. ! What is a light year? ! How long would it take to reach the nearest star to our solar system? (Image Credit: NASA/Transition Region & Coronal Explorer) Note: The above image of the Sun is an X -ray view rather than a visible light image. Stellar Distances Teacher Guide In this exercise students will plan a scale model to explore the distances between stars, focusing on Alpha Centauri, the system of stars nearest to the Sun. This activity builds upon the activity Sizes of Stars, which should be done first, and upon the Scale in the Solar System activity, which is strongly recommended as a prerequisite. Stellar Distances is a math activity as well as a science activity. Necessary Prerequisite: Sizes of Stars activity Recommended Prerequisite: Scale Model Solar System activity Grade Level: 6-8 Curriculum Standards: The Stellar Distances lesson is matched to: ! National Science and Math Education Content Standards for grades 5-8. ! National Math Standards 5-8 ! Texas Essential Knowledge and Skills (grades 6 and 8) ! Content Standards for California Public Schools (grade 8) Time Frame: The activity should take approximately 45 minutes to 1 hour to complete, including short introductions and follow-ups. Purpose: To aid students in understanding the distances between stars, how those distances compare with the sizes of stars, and the distances between objects in our own solar system. © 2007 Dr Mary Urquhart, University of Texas at Dallas Stars and Planets 2 TEACHER GUIDE Stellar Distances Key Concepts: o Distances between stars are immense compared with the sizes of stars.