DOCSLIB.ORG

1) the Case for Stochastic Orbital Migration 2) Open Exoplanet Catalogue

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Institute for Advanced Study 1) The case for stochastic orbital migration 2) Open Exoplanet Catalogue Hanno Rein @ UoT St. George Campus, March 2013 Extra-solar planet census All discovered extra-solar planets 869 confirmed extra- solar planets • Super-Jupiters • (Hot) Jupiters • Neptunes • Super-Earths • Earth-like planets Open Exoplanet Catalogue (Rein 2012b) All multi-planetary systems 327 confirmed planets in multi-planetary systems • Multiple Jupiters • Densely packed systems of Neptunes and (Super)-Earths • 1 Solar System • Some systems are deep in resonance Open Exoplanet Catalogue (Rein 2012b) Radial velocity planets 80 RV planets 70 Cumulative period ] 60 ratio in multi- 10 jup [M planetary systems 2 50 + m 1 • Periods of systems with 40 massive planets tend to pile up near integer number of pairs 30 ratios 1 20 total planet mass m • Most prominent 10 features at 4:1, 3:1, 2:1, 0 3:2 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio 300 0.1 KOI planets 250 ] jup [M Rein, Payne, Veras & Ford (2012) 200 2 + m 1 150 number of pairs 100 total planet mass m 50 0 0.01 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio Kepler candidates 2740 planet candidates • Probing a different regime • Small mass planets • A lot of planets Open Exoplanet Catalogue (Rein 2012b) Kepler candidates with multiple planets Kepler multi-planetary systems • Small mass planets • Hierarchical systems • Densely packed • Not many are in resonance Open Exoplanet Catalogue (Rein 2012b) 80 RV planets 70 ] 60 10 jup [M 2 50 + m 1 40 number of pairs 30 1 20 total planet mass m Kepler's 10 transiting planet candidates 0 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio 300 0.1 KOI planets 250 • Period ratio ] jup distribution much [M 200 2 smoother for small + m mass planets 1 150 • Deficiencies near 4:3, number of pairs 3:2, 2:1 100 total planet mass m • Excess slightly outside 50 of the exact commensurability 0 0.01 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio Rein, Payne, Veras & Ford (2012) Stochastic orbital migration Migration - Type I • Low mass planets • No gap opening in disc • Migration rate is fast • Depends strongly on thermodynamics of the disc 2D hydro code Prometheus (Rein 2010) Migration - Type II • Massive planets (typically bigger than Saturn) • Opens a (clear) gap • Migration rate is slow • Follows viscous evolution of the disc 2D hydro code Prometheus (Rein 2010) How does a real protoplanetary disk look like? Image credit: NASA/JPL-Caltech Why think about stochastic migration? • Angular momentum transport • Magnetorotational instability (MRI) • Density perturbations interact gravitationally with planets • Stochastic forces lead to random walk • Large uncertainties in strength of forces Animation from Nelson & Papaloizou 2004 Random forces measured by Laughlin et al. 2004, Nelson 2005, Oischi et al. 2007 Random walk in all orbital parameters pericenter eccentricity semi-major axis time Rein & Papaloizou 2009 Analytic growth rates for 1 planet 0.01 Dt 2 [AU] 0.001 (∆a) =4 RMS a> 2 n < 0.0001 1 2 2.5 γDt 0.1 RMS (∆$) = > 2 2 2 < e n a 0.01 0.001 0.01 γDt RMS 2 0.001 e> (∆e) =2.5 < n2a2 0.0001 Simulations Analytic solution Analytic solution (=1) 10 100 1000 10000 100000 time [years] Rein & Papaloizou 2009, Adams et al 2009, Rein 2010 Analytic growth rates for 2 planets 2 (∆⇥1) 9γf 2 = 2 2 Dt (p + 1) a1⇤lf 2 5γs (∆(∆⌅)) = 2 2 2 Dt 4a1n1e1 Rein & Papaloizou 2009 Multi-planetary systems in mean motion resonance GJ876 Earth • Stability of multi-planetary systems depends strongly on diffusion coefficient • Most planetary systems are stable for entire disc lifetime Rein & Papaloizou 2009 The formation of Kepler-36 Kepler-36 c as seen from Kepler-36 b • Would appear 2.5 times the size of the Moon • Very close orbits, near a 7:6 resonance • Very different densities Formation of Kepler-36 2.8 • Migration rate and mass 106 ratio determine the final 2.6 resonance stable resonances 2.4 105 8:7 7:6 6:5 5:4 4:3 3:2 Higher order resonances 2.2 • require faster migration 2.0 rates 104 1.8 time [yrs] period ratio • Higher mass planets end up crossing of the 2:1 resonance 1.6 in lower order resonances 103 1.4 • Once in resonance, planets convergent migration 1.2 often stay there for the rest 102 of the disc lifetime 1.0 103 104 105 migration timescale [yrs] Pardekooper, Rein & Kley (in prep) Problem with Kepler-36 <1000 years Need extremely fast migration rate to capture into a high order resonance. Unrealistically fast. Planets are not large enough to migrate in Type III regime. Pardekooper, Rein & Kley (in prep) τa = 2000 yrs τa = 10000 yrs low order resonances low order resonances high order resonances 2.8 2.8 104 7:6 2.6 2.6 2.4 5:4 2.4 104 2.2 2.2 3:2 2.0 2.0 103 1.8 1.8 time [yrs] time [yrs] period ratio 3 period ratio crossing of the 2:1 resonance 1.6 10 crossing of the 2:1 resonance 1.6 1.4 1.4 102 convergent migration 1.2 convergent migration 1.2 1.0 1.0 Solution: Stochastic10-3 migration10-2 10-1 10-3 10-2 10-1 amplitude of stochastic forces [F0] amplitude of stochastic forces [F0] τa = 20000 yrs τa = 100000 yrs low order resonances high order resonances low order resonances high order resonances 2.8 2.8 105 2.6 2.6 4:3 4:3 2.4 2.4 105 2.2 2.2 3:2 3:2 104 2.0 2.0 1.8 1.8 time [yrs] time [yrs] period ratio 104 period ratio crossing of the 2:1 resonance 1.6 crossing of the 2:1 resonance 1.6 103 1.4 1.4 convergent migration 1.2 convergent migration 1.2 1.0 103 1.0 10-3 10-2 10-1 10-3 10-2 10-1 amplitude of stochastic forces [F0] amplitude of stochastic forces [F0] Pardekooper, Rein & Kley (in prep) A statistical analysis 80 RV planets 70 ] 60 10 jup [M 2 50 + m 1 40 number of pairs 30 1 20 total planet mass m Kepler's 10 transiting planet candidates 0 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio 300 0.1 KOI planets 250 • Period ratio ] jup distribution much [M 200 2 smoother for small + m mass planets 1 150 • Deficiencies near 4:3, number of pairs 3:2, 2:1 100 total planet mass m • Excess slightly outside 50 of the exact commensurability 0 0.01 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio Rein, Payne, Veras & Ford (2012) Testing stochastic migration: Method Architecture and masses from observed KOIs Placing planets in a MMSN, further out, further apart, randomizing all angles N-body simulation with migration forces Rein 2012 Testing stochastic migration: Advantages Comparison of Comparison of statistical quantities individual systems • Period ratio distribution • Especially interesting for • Eccentricity distribution multi-planetary systems • TTVs • Can create multiple realizations of each system No synthesis of a planet population required • Observed masses, architectures • Model independent Preliminary results 600 Observed KOI planets 4 -6 Migration τ =10 years, α=10 a 4 -5 Migration τ =10 years, α=10 500 a 400 300 300 number of pairs 200 250 100 200 1.9 2 2.1 0 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio Rein 2012 Future expansions Physical disk model Completeness • 1D hydrodynamic simulation • Include planets missed by Kepler • Coupled to N-body simulations GPU based integrators Other physical effects • Allows for much bigger samples • Tidal damping • Wider parameter space exploration • Evaporation Saturn’s Rings REBOUND • Code description paper published by A&A, Rein & Liu 2012 • Multi-purpose N-body code • Only public N-body code that can be used for granular dynamics Astronomy & Astrophysics manuscript no. paper c ESO 2011 October 20, 2011 • Written in C99, open source, GPL REBOUND: An open-source multi-purpose N-body code for collisional dynamics Hanno Rein 1 and Shang-Fei Liu 2,3 • 1 Institute for Advanced Study, 1 Einstein Drive, Princeton, NJ 08540 Freely available at e-mail: [email protected] 2 Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, P. R. China 3 Department of Astronomy, Peking University, Beijing 100871, P. R. China e-mail: [email protected] http://github.com/hannorein/rebound Submitted: 13 September 2011 ABSTRACT REBOUND is a new multi-purpose N-body code which is freely available under an open-source license. It was designed for collisional dynamics such as planetary rings but can also solve the classical N-body problem. It is highly modular and can be customized easily to work on a wide variety of di ↵erent problems in astrophysics and beyond. REBOUND comes with three symplectic integrators: leap-frog, the symplectic epicycle integrator (SEI) and a Wisdom-Holman mapping (WH). It supports open, periodic and shearing-sheet boundary conditions. REBOUND can use a Barnes-Hut tree to calculate both self- gravity and collisions. These modules are fully parallelized with MPI as well as OpenMP. The former makes use of a static domain decomposition and a distributed essential tree. Two new collision detection modules based on a plane-sweep algorithm are also implemented.
Recommended publications
  • IAU Division C Working Group on Star Names 2019 Annual Report

    IAU Division C Working Group on Star Names 2019 Annual Report

    IAU Division C Working Group on Star Names 2019 Annual Report Eric Mamajek (chair, USA) WG Members: Juan Antonio Belmote Avilés (Spain), Sze-leung Cheung (Thailand), Beatriz García (Argentina), Steven Gullberg (USA), Duane Hamacher (Australia), Susanne M. Hoffmann (Germany), Alejandro López (Argentina), Javier Mejuto (Honduras), Thierry Montmerle (France), Jay Pasachoff (USA), Ian Ridpath (UK), Clive Ruggles (UK), B.S. Shylaja (India), Robert van Gent (Netherlands), Hitoshi Yamaoka (Japan) WG Associates: Danielle Adams (USA), Yunli Shi (China), Doris Vickers (Austria) WGSN Website: https://www.iau.org/science/scientific_bodies/working_groups/280/ ​ WGSN Email: [email protected] ​ The Working Group on Star Names (WGSN) consists of an international group of astronomers with expertise in stellar astronomy, astronomical history, and cultural astronomy who research and catalog proper names for stars for use by the international astronomical community, and also to aid the recognition and preservation of intangible astronomical heritage. The Terms of Reference and membership for WG Star Names (WGSN) are provided at the IAU website: https://www.iau.org/science/scientific_bodies/working_groups/280/. ​ ​ ​ WGSN was re-proposed to Division C and was approved in April 2019 as a functional WG whose scope extends beyond the normal 3-year cycle of IAU working groups. The WGSN was specifically called out on p. 22 of IAU Strategic Plan 2020-2030: “The IAU serves as the ​ internationally recognised authority for assigning designations to celestial bodies and their surface features. To do so, the IAU has a number of Working Groups on various topics, most notably on the nomenclature of small bodies in the Solar System and planetary systems under Division F and on Star Names under Division C.” WGSN continues its long term activity of researching cultural astronomy literature for star names, and researching etymologies with the goal of adding this information to the WGSN’s online materials.
  • Tabetha Boyajian's CV

    Tabetha Boyajian's CV

    Dr. Tabetha Boyajian Yale University, Department of Astronomy, 52 Hillhouse Ave., New Haven, CT 06520 USA [email protected] • +1 (404) 849-4848 • http://www.astro.yale.edu/tabetha PROFESSIONAL Yale University, Department of Astronomy, New Haven, Connecticut, USA EXPERIENCE Postdoctoral Fellow 2012 – present • Supervisor: Dr. Debra Fischer Center for high Angular Resolution Astronomy (CHARA), Georgia State University Hubble Fellow 2009 – 2012 • Supervisor: Dr. Harold McAlister EDUCATION Georgia State University, Department of Physics and Astronomy, Atlanta, Georgia, USA Doctor of Philosophy (Ph.D.) in Astronomy 2005 – 2009 • Adviser: Dr. Harold McAlister Master of Science (M.S.) in Physics 2003 – 2005 • Adviser: Dr. Douglas Gies College of Charleston, Charleston, South Carolina, USA Bachelor of Science (B.S.) in Physics with concentration in astronomy 1998 – 2003 • Graduated with Departmental Honors PROFESSIONAL Secretary, International Astronomical Union, Division G 2015 – 2018 SERVICE Steering Committee, International Astronomical Union, Division G 2015 – 2018 Review panel member NASA Kepler Guest Observer program, NASA K2 Guest Observer program, NSF-AAG program Referee The Astronomical Journal, Astronomy & Astrophysics, PASA Telescope time allocation committee member CHARA, OPTICON (external) AREAS OF Fundamental properties of stars: diameters, temperatures, exoplanet detection and characterization, SPECIALIZATION Optical/IR interferometry, stellar spectroscopy (radial velocities, abundances, activity), absolute AND INTEREST
  • 2019 Destination Imagination Global Finals Escape Artists Results File:///C:/Users/Tinas/Desktop/GF19 Results/Tournamentresults-ESCAPE

    2019 Destination Imagination Global Finals Escape Artists Results File:///C:/Users/Tinas/Desktop/GF19 Results/Tournamentresults-ESCAPE

    2019 Destination Imagination Global Finals Escape Artists Results file:///C:/Users/tinas/Desktop/GF19 results/TournamentResults-ESCAPE... Destination Imagination congratulates all the students who participated in the Kansas City tournament. We think you are all winners! Teams emphasized as such are going on to the next level of competition. pO: Escape Artists, Elementary Level Total Central Choice Instant Rank Name Town Mbrshp# Deduct Rw. Cen Rw.TCE RwInst Tragic Magic, 359.07 240.00 60.00 59.07 1 Deerfield, Illinois 114-87177 Walden - DPS 109 0.00 198.53 52.28 53.75 Whitestone 1- 352.04 211.63 54.97 85.44 2 Quirky Queens, LEANDER ISD, Texas 750-63539 WHITESTONE EL 0.00 175.06 47.90 77.75 Superior 7, Zue 339.94 192.44 49.97 97.53 3 Bales Intermediate Friendswood ISD, Texas 750-05676 School 0.00 159.19 43.54 88.75 Chalk It Up!, 337.90 196.21 45.54 96.15 4 WYLIE ISD, Texas 750-27357 WYLIE INT 0.00 162.31 39.68 87.50 Creative Crayons, PFLUGERVILLE ISD, 326.94 208.27 49.99 68.68 5 750-77238 TIMMERMAN EL Texas 0.00 172.28 43.56 62.50 Service Ninjas, MIDLOTHIAN ISD, 323.01 209.34 55.70 57.97 6 750-31300 Miller Elementary Texas 0.00 173.17 48.53 52.75 Hurricane Helpers, 317.64 179.13 39.88 98.63 7 Terrace Park - 5th Terrace Park, Ohio 135-63707 grade Buchholz 0.00 148.18 34.75 89.75 The Spicy DI ritos, 315.12 216.97 45.40 52.75 8 KLEIN ISD, Texas 750-92814 METZLER EL 0.00 179.48 39.56 48.00 Fantastic 5, 313.69 193.77 39.70 80.22 9 Warren, Ohio 135-81882 Howland LSD 0.00 160.29 34.59 73.00 Screaming Main 310.36 176.29 36.82 97.25 Melody, Beijing 10 China 185-63578 Huilongguan YuXin 0.00 145.83 32.08 88.50 Sch of CNU 11T The Care Crew, St.
  • 1) the Case for Stochastic Orbital Migration 2) Open Exoplanet Catalogue

    1) the Case for Stochastic Orbital Migration 2) Open Exoplanet Catalogue

    Institute for Advanced Study 1) The case for stochastic orbital migration 2) Open Exoplanet Catalogue Hanno Rein @ CITA, March 2013 Extra-solar planet census All discovered extra-solar planets 869 confirmed extra- solar planets • Super-Jupiters • (Hot) Jupiters • Neptunes • Super-Earths • Earth-like planets Open Exoplanet Catalogue (Rein 2012b) All multi-planetary systems 327 confirmed planets in multi-planetary systems • Multiple Jupiters • Densely packed systems of Neptunes and (Super)-Earths • 1 Solar System • Some systems are deep in resonance Open Exoplanet Catalogue (Rein 2012b) Radial velocity planets 80 RV planets 70 Cumulative period ] 60 ratio in multi- 10 jup [M planetary systems 2 50 + m 1 • Periods of systems with 40 massive planets tend to pile up near integer number of pairs 30 ratios 1 20 total planet mass m • Most prominent 10 features at 4:1, 3:1, 2:1, 0 3:2 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio 300 0.1 KOI planets 250 ] jup [M Rein, Payne, Veras & Ford (2012) 200 2 + m 1 150 number of pairs 100 total planet mass m 50 0 0.01 1 1.33 1.5 2 3 4 5 6 7 8 9 period ratio Kepler candidates 2740 planet candidates • Probing a different regime • Small mass planets • A lot of planets Open Exoplanet Catalogue (Rein 2012b) Kepler candidates with multiple planets Kepler multi-planetary systems • Small mass planets • Hierarchical systems • Densely packed • Not many are in resonance Open Exoplanet Catalogue (Rein 2012b) 80 RV planets 70 ] 60 10 jup [M 2 50 + m 1 40 number of pairs 30 1 20 total planet mass m Kepler's 10 transiting planet
  • Pos(BASH2015)007

    Pos(BASH2015)007

    Precision Stellar Astrophysics in the Kepler Era PoS(BASH2015)007 Daniel Huber∗ Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia E-mail: [email protected] The study of fundamental properties (such as temperatures, radii, masses, and ages) and interior processes (such as convection and angular momentum transport) of stars has implications on var- ious topics in astrophysics, ranging from the evolution of galaxies to understanding exoplanets. In this contribution I will review the basic principles of two key observational methods for con- straining fundamental and interior properties of single field stars: the study stellar oscillations (asteroseismology) and optical long-baseline interferometry. I will highlight recent breakthrough discoveries in asteroseismology such as the measurement of core rotation rates in red giants and the characterization of exoplanet systems. I will furthermore comment on the reliability of inter- ferometry as a tool to calibrate indirect methods to estimate fundamental properties, and present a new angular diameter measurement for the exoplanet host star HD 219134 which demonstrates that diameters for stars which are relatively well resolved (& 1 mas for the K band) are consistent across different instruments. Finally I will discuss the synergy between asteroseismology and interferometry to test asteroseismic scaling relations, and give a brief outlook on the expected impact of space-based missions such as K2, TESS and Gaia. Frank N. Bash Symposium 2015 18-20 October The University of Texas at Austin, USA ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0).
  • A New Interferometric Study of Four Exoplanet Host Stars: Θ Cygni, 14 Andromedae, Υ Andromedae and 42 Draconis,

    A New Interferometric Study of Four Exoplanet Host Stars: Θ Cygni, 14 Andromedae, Υ Andromedae and 42 Draconis,

    A&A 545, A5 (2012) Astronomy DOI: 10.1051/0004-6361/201219467 & c ESO 2012 Astrophysics A new interferometric study of four exoplanet host stars: θ Cygni, 14 Andromedae, υ Andromedae and 42 Draconis, R. Ligi1, D. Mourard1,A.M.Lagrange2,K.Perraut2, T. Boyajian4,, Ph. Bério1,N.Nardetto1, I. Tallon-Bosc3, H. McAlister4,5, T. ten Brummelaar4,S.Ridgway6, J. Sturmann4, L. Sturmann4,N.Turner4, C. Farrington4, and P. J. Goldfinger4 1 Laboratoire Lagrange, UMR 7293 UNS-CNRS-OCA, Boulevard de l’Observatoire, BP 4229, 06304 Nice Cedex 4, France e-mail: [email protected] 2 UJF-Grenoble1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble, UMR 5274, 38041 Grenoble, France 3 UCBL/CNRS CRAL, 9 avenue Charles André, 69561 Saint-Genis-Laval Cedex, France 4 Georgia State University, PO Box 3969, Atlanta GA 30302-3969, USA 5 CHARA Array, Mount Wilson Observatory, 91023 Mount Wilson CA, USA 6 National Optical Astronomy Observatory, PO Box 26732, Tucson, AZ 85726, USA Received 24 April 2012 / Accepted 25 June 2012 ABSTRACT Context. Since the discovery of the first exoplanet in 1995 around a solar-type star, the interest in exoplanetary systems has kept increasing. Studying exoplanet host stars is of the utmost importance to establish the link between the presence of exoplanets around various types of stars and to understand the respective evolution of stars and exoplanets. Aims. Using the limb-darkened diameter (LDD) obtained from interferometric data, we determine the fundamental parameters of four exoplanet host stars. We are particularly interested in the F4 main-sequence star, θ A&A 545, A5 (2012) array at Mount Wilson, California (ten Brummelaar et al.
  • Extrasolar Planets and Their Host Stars

    Extrasolar Planets and Their Host Stars

    Kaspar von Braun & Tabetha S. Boyajian Extrasolar Planets and Their Host Stars July 25, 2017 arXiv:1707.07405v1 [astro-ph.EP] 24 Jul 2017 Springer Preface In astronomy or indeed any collaborative environment, it pays to figure out with whom one can work well. From existing projects or simply conversations, research ideas appear, are developed, take shape, sometimes take a detour into some un- expected directions, often need to be refocused, are sometimes divided up and/or distributed among collaborators, and are (hopefully) published. After a number of these cycles repeat, something bigger may be born, all of which one then tries to simultaneously fit into one’s head for what feels like a challenging amount of time. That was certainly the case a long time ago when writing a PhD dissertation. Since then, there have been postdoctoral fellowships and appointments, permanent and adjunct positions, and former, current, and future collaborators. And yet, con- versations spawn research ideas, which take many different turns and may divide up into a multitude of approaches or related or perhaps unrelated subjects. Again, one had better figure out with whom one likes to work. And again, in the process of writing this Brief, one needs create something bigger by focusing the relevant pieces of work into one (hopefully) coherent manuscript. It is an honor, a privi- lege, an amazing experience, and simply a lot of fun to be and have been working with all the people who have had an influence on our work and thereby on this book. To quote the late and great Jim Croce: ”If you dig it, do it.
  • Full Program

    Full Program

    1 Schedule Abstracts Author Index 2 Schedule Schedule ............................................................................................................................... 3 Abstracts ............................................................................................................................... 5 Monday, September 12, 2011, 8:30 AM - 10:00 AM ................................................................................ 5 01: Overview of Observations and Welcome ....................................................................................... 5 Monday, September 12, 2011, 10:30 AM - 12:00 PM .............................................................................. 7 02: Radial Velocities ............................................................................................................................. 7 Monday, September 12, 2011, 2:00 PM - 3:30 PM ................................................................................ 10 03: Transiting Planets ......................................................................................................................... 10 Monday, September 12, 2011, 4:00 PM - 5:30 PM ................................................................................ 13 04: Transiting Planets II ...................................................................................................................... 13 Tuesday, September 13, 2011, 8:30 AM - 10:00 AM .............................................................................. 16 05: Planets
  • !Meteor News Cover [Vol 4

    !Meteor News Cover [Vol 4

    2020 – 5 eMeteorNews Contents Obituary Oleg Igorevich Belkovich (1934 – 2020) Galina Ryabova ....................................................................................................................................... 285 Possible upcoming return of the chi Cygnids in September 2020 Peter Jenniskens ...................................................................................................................................... 287 Meteors and 2018 LF5 John Greaves ........................................................................................................................................... 290 Some Near Earth Object and meteor associations John Greaves ........................................................................................................................................... 295 Results of spectral observations of meteor showers and sporadic meteors from October 2018 until May 2020 Takashi Sekiguchi .................................................................................................................................... 300 The Lyrids and a minor antihelion outburst in 2020 Thomas Weiland ...................................................................................................................................... 314 Lyrids 2020: successful campaign! Koen Miskotte .......................................................................................................................................... 317 Meteor observations from Midden-Eierland on the Dutch island of Texel Koen
  • Sirius Astronomer Newsletter

    Sirius Astronomer Newsletter

    February 2016 Free to members, subscriptions $12 for 12 issues Volume 43, Number 2 The Milky Way looms bright over the Owens Valley Radio Observatory in this picture taken by Pauline Acalin during a recent OCA field trip to the facility. Owens Valley is one of several field trips the club conducts on a regular basis. Be sure to check our website for details about upcoming trips! OCA CLUB MEETING STAR PARTIES COMING UP The free and open club meeting will The Black Star Canyon site will open on The next session of the Beginners be held February 12 at 7:30 PM in the February 13 and March 5. The Anza site will Class will be held at the Heritage Mu- Irvine Lecture Hall of the Hashinger be open on February 6 and March 5. Mem- seum of Orange County at 3101 West Science Center at Chapman University bers are encouraged to check the website Harvard Street in Santa Ana on Febru- in Orange. This month’s speaker is calendar for the latest updates on star par- ary 5. The following class will be held Jerome Orosz of San Diego State Uni- ties and other events. March 4. versity with the topic “Planets With Two Suns” Please check the website calendar for the GOTO SIG: TBA outreach events this month! Volunteers are Astro-Imagers SIG: Feb. 9, Mar. 8 NEXT MEETINGS: Mar. 11, Apr. 8 always welcome! Remote Telescopes: TBA Astrophysics SIG: Feb. 19, Mar. 18 You are also reminded to check the web Dark Sky Group: TBA site frequently for updates to the calendar of events and other club news.
  • Michael Carroll How We Find Them, Communicate with Them, And

    Michael Carroll How We Find Them, Communicate with Them, And

    Michael Carroll Earths of Distant Suns How We Find Them, Communicate with Them, and Maybe Even Travel There Earths of Distant Suns Michael Carroll Earths of Distant Suns How We Find Them, Communicate with Them, and Maybe Even Travel There Michael Carroll Fellow, International Association of Astronomical Artists Littleton , CO , USA ISBN 978-3-319-43963-1 ISBN 978-3-319-43964-8 (eBook) DOI 10.1007/978-3-319-43964-8 Library of Congress Control Number: 2016951720 © Springer International Publishing Switzerland 2017 Th is work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifi cally the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfi lms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. Th e use of general descriptive names, registered names, trademarks, service marks, etc. in this publication does not imply, even in the absence of a specifi c statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. Th e publisher, the authors and the editors are safe to assume that the advice and information in this book are believed to be true and accurate at the date of publication. Neither the publisher nor the authors or the editors give a warranty, express or implied, with respect to the material contained herein or for any errors or omissions that may have been made.
  • Precision Stellar Astrophysics in the Kepler Era Daniel Huber

    Precision Stellar Astrophysics in the Kepler Era Daniel Huber

    Precision Stellar Astrophysics in the Kepler Era Daniel Huber∗ Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Australia E-mail: [email protected] The study of fundamental properties (such as temperatures, radii, masses, and ages) and interior processes (such as convection and angular momentum transport) of stars has implications on var- ious topics in astrophysics, ranging from the evolution of galaxies to understanding exoplanets. In this contribution I will review the basic principles of two key observational methods for con- straining fundamental and interior properties of single field stars: the study stellar oscillations (asteroseismology) and optical long-baseline interferometry. I will highlight recent breakthrough discoveries in asteroseismology such as the measurement of core rotation rates in red giants and the characterization of exoplanet systems. I will furthermore comment on the reliability of inter- ferometry as a tool to calibrate indirect methods to estimate fundamental properties, and present a new angular diameter measurement for the exoplanet host star HD219134 which demonstrates that diameters for stars which are relatively well resolved (& 1mas for the K band) are consistent across different instruments. Finally I will discuss the synergy between asteroseismology and interferometry to test asteroseismic scaling relations, and give a brief outlook on the expected impact of space-based missions such as K2, TESS and Gaia. arXiv:1604.07442v1 [astro-ph.SR] 25 Apr 2016 Frank N. Bash Symposium 2015 18-20 October The University of Texas at Austin, USA ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0).