CESRA Workshop 2019: the Sun and the Inner Heliosphere Programme
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Our Dynamic Sun: 2017 Hannes Alfvén Medal Lecture at the EGU
Ann. Geophys., 35, 805–816, 2017 https://doi.org/10.5194/angeo-35-805-2017 © Author(s) 2017. This work is distributed under the Creative Commons Attribution 3.0 License. Our dynamic sun: 2017 Hannes Alfvén Medal lecture at the EGU Eric Priest1,* 1Mathematics Institute, St Andrews University, St Andrews KY16 9SS, UK *Invited contribution by Eric Priest, recipient of the EGU Hannes Alfvén Medal for Scientists 2017 Correspondence to: Eric Priest ([email protected]) Received: 15 May 2017 – Accepted: 12 June 2017 – Published: 14 July 2017 Abstract. This lecture summarises how our understanding 1 Introduction of many aspects of the Sun has been revolutionised over the past few years by new observations and models. Much of the Thank you most warmly for the award of the Alfvén Medal, dynamic behaviour of the Sun is driven by the magnetic field which gives me great pleasure. In addition to a feeling of since, in the outer atmosphere, it represents the largest source surprise, I am also deeply humbled, because Alfvén was one of energy by far. of the greats in the field and one of my heroes as a young The interior of the Sun possesses a strong shear layer at the researcher (Fig. 1). We need dedicated scientists who fol- base of the convection zone, where sunspot magnetic fields low a specialised topic with tenacity and who complement are generated. A small-scale dynamo may also be operating one another in our amazingly diverse field; but we also need near the surface of the Sun, generating magnetic fields that time and space for creativity in this busy world, especially thread the lowest layer of the solar atmosphere, the turbulent for those princes of creativity, mavericks like Alfvén who can photosphere. -
Large-Scale Periodic Solar Velocities
LARGE-SCALE PERIODIC SOLAR VELOCITIES: AN OBSERVATIONAL STUDY (NASA-CR-153256) LARGE-SCALE PERIODIC SOLAR N77-26056 ElOCITIeS: AN OBSERVATIONAL STUDY Stanford Univ.) 211 p HC,A10/F A01 CSCL 03B Unclas G3/92 35416 by Phil Howard Dittmer Office of Naval Research Contract N00014-76-C-0207 National Aeronautics and Space Administration Grant NGR 05-020-559 National Science Foundation Grant ATM74-19007 Grant DES75-15664 and The Max C.Fleischmann Foundation SUIPR Report No. 686 T'A kj, JUN 1977 > March 1977 RECEIVED NASA STI FACILITY This document has been approved for public INPUT B N release and sale; its distribution isunlimited. 4 ,. INSTITUTE FOR PLASMA RESEARCH STANFORD UNIVERSITY, STANFORD, CALIFORNIA UNCLASSIFIED SECURITY CLASSIFICATION OF THIS PAGE (When Data Entered) DREAD INSTRUCTIONS REPORT DOCUMENTATION PAGE BEFORE COMPLETING FORM I- REPORT NUMBER 2 GOVT ACCESSION NO. 3. RECIPIENT'S CATALOG NUMBER SUIPR Report No. 686 4. TITLE (and Subtitle) 5 TYPE OF REPORT & PERIOD COVERED Large-Scale Periodic Solar Velocities: Scientific, Technical An Observational Study 6. PERFORMING ORG. REPORT NUMBER 7. AUTHOR(s) 8 CONTRACT OR GRANT NUMBER(s) Phil Howard Dittmer N00014-76-C-0207 S PERFORMING ORGANIZATION NAME AND ADDRESS 10. PROGRAM ELEMENT, PROJECT, TASK Institute for Plasma Research AREA & WORK UNIT NUMBERS Stanford University Stanford, California 94305 12. REPORT DATE . 13. NO. OF PAGES 11. CONTROLLING OFFICE NAME AND ADDRESS March 1977 211 Office of Naval Research Electronics Program Office 15. SECURITY CLASS. (of-this report) Arlington, Virginia 22217 Unclassified 14. MONITORING AGENCY NAME & ADDRESS (if diff. from Controlling Office) 15a. DECLASSIFICATION/DOWNGRADING SCHEDULE 16. DISTRIBUTION STATEMENT (of this report) This document has been approved for public release and sale; its distribution is unlimited. -
Detecting Differential Rotation and Starspot Evolution on the M Dwarf GJ 1243 with Kepler James R
Western Washington University Masthead Logo Western CEDAR Physics & Astronomy College of Science and Engineering 6-20-2015 Detecting Differential Rotation and Starspot Evolution on the M Dwarf GJ 1243 with Kepler James R. A. Davenport Western Washington University, [email protected] Leslie Hebb Suzanne L. Hawley Follow this and additional works at: https://cedar.wwu.edu/physicsastronomy_facpubs Part of the Stars, Interstellar Medium and the Galaxy Commons Recommended Citation Davenport, James R. A.; Hebb, Leslie; and Hawley, Suzanne L., "Detecting Differential Rotation and Starspot Evolution on the M Dwarf GJ 1243 with Kepler" (2015). Physics & Astronomy. 16. https://cedar.wwu.edu/physicsastronomy_facpubs/16 This Article is brought to you for free and open access by the College of Science and Engineering at Western CEDAR. It has been accepted for inclusion in Physics & Astronomy by an authorized administrator of Western CEDAR. For more information, please contact [email protected]. The Astrophysical Journal, 806:212 (11pp), 2015 June 20 doi:10.1088/0004-637X/806/2/212 © 2015. The American Astronomical Society. All rights reserved. DETECTING DIFFERENTIAL ROTATION AND STARSPOT EVOLUTION ON THE M DWARF GJ 1243 WITH KEPLER James R. A. Davenport1, Leslie Hebb2, and Suzanne L. Hawley1 1 Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA; [email protected] 2 Department of Physics, Hobart and William Smith Colleges, Geneva, NY 14456, USA Received 2015 March 9; accepted 2015 May 6; published 2015 June 18 ABSTRACT We present an analysis of the starspots on the active M4 dwarf GJ 1243, using 4 years of time series photometry from Kepler. -
Starspot Temperature Along the HR Diagram
Mem. S.A.It. Suppl. Vol. 9, 220 Memorie della c SAIt 2006 Supplementi Starspot temperature along the HR diagram K. Biazzo1, A. Frasca2, S. Catalano2, E. Marilli2, G. W. Henry3, and G. Tasˇ 4 1 Department of Physics and Astronomy, University of Catania, via Santa Sofia 78, 95123 Catania, e-mail: [email protected] 2 INAF - Catania Astrophysical Observatory, via S. Sofia 78, 95123 Catania, Italy 3 Tennessee State University - Center of Excellence in Information Systems, 330 10th Ave. North, Nashville, TN 37203-3401 4 Ege University Observatory - 35100 Bornova, Izmir˙ , Turkey Abstract. The photospheric temperature of active stars is affected by the presence of cool starspots. The determination of the spot configuration and, in particular, spot temperatures and sizes, is important for understanding the role of the magnetic field in blocking the convective heating flux inside starspots. It has been demonstrated that a very sensitive di- agnostic of surface temperature in late-type stars is the depth ratio of weak photospheric absorption lines (e.g. Gray & Johanson 1991, Catalano et al. 2002). We have shown that it is possible to reconstruct the distribution of the spots, along with their sizes and tempera- tures, from the application of a spot model to the light and temperature curves (Frasca et al. 2005). In this work, we present and briefly discuss results on spot sizes and temperatures for stars in various locations in the HR diagram. Key words. Stars: activity - Stars: variability - Stars: starspot 1. Introduction Table 1. Star sample. Within a large program aimed at studying the behaviour of photospheric surface inhomo- Star Sp. -
Abstracts Connecting to the Boston University Network
20th Cambridge Workshop: Cool Stars, Stellar Systems, and the Sun July 29 - Aug 3, 2018 Boston / Cambridge, USA Abstracts Connecting to the Boston University Network 1. Select network ”BU Guest (unencrypted)” 2. Once connected, open a web browser and try to navigate to a website. You should be redirected to https://safeconnect.bu.edu:9443 for registration. If the page does not automatically redirect, go to bu.edu to be brought to the login page. 3. Enter the login information: Guest Username: CoolStars20 Password: CoolStars20 Click to accept the conditions then log in. ii Foreword Our story starts on January 31, 1980 when a small group of about 50 astronomers came to- gether, organized by Andrea Dupree, to discuss the results from the new high-energy satel- lites IUE and Einstein. Called “Cool Stars, Stellar Systems, and the Sun,” the meeting empha- sized the solar stellar connection and focused discussion on “several topics … in which the similarity is manifest: the structures of chromospheres and coronae, stellar activity, and the phenomena of mass loss,” according to the preface of the resulting, “Special Report of the Smithsonian Astrophysical Observatory.” We could easily have chosen the same topics for this meeting. Over the summer of 1980, the group met again in Bonas, France and then back in Cambridge in 1981. Nearly 40 years on, I am comfortable saying these workshops have evolved to be the premier conference series for cool star research. Cool Stars has been held largely biennially, alternating between North America and Europe. Over that time, the field of stellar astro- physics has been upended several times, first by results from Hubble, then ROSAT, then Keck and other large aperture ground-based adaptive optics telescopes. -
10. Scientific Programme 10.1
10. SCIENTIFIC PROGRAMME 10.1. OVERVIEW (a) Invited Discourses Plenary Hall B 18:00-19:30 ID1 “The Zoo of Galaxies” Karen Masters, University of Portsmouth, UK Monday, 20 August ID2 “Supernovae, the Accelerating Cosmos, and Dark Energy” Brian Schmidt, ANU, Australia Wednesday, 22 August ID3 “The Herschel View of Star Formation” Philippe André, CEA Saclay, France Wednesday, 29 August ID4 “Past, Present and Future of Chinese Astronomy” Cheng Fang, Nanjing University, China Nanjing Thursday, 30 August (b) Plenary Symposium Review Talks Plenary Hall B (B) 8:30-10:00 Or Rooms 309A+B (3) IAUS 288 Astrophysics from Antarctica John Storey (3) Mon. 20 IAUS 289 The Cosmic Distance Scale: Past, Present and Future Wendy Freedman (3) Mon. 27 IAUS 290 Probing General Relativity using Accreting Black Holes Andy Fabian (B) Wed. 22 IAUS 291 Pulsars are Cool – seriously Scott Ransom (3) Thu. 23 Magnetars: neutron stars with magnetic storms Nanda Rea (3) Thu. 23 Probing Gravitation with Pulsars Michael Kremer (3) Thu. 23 IAUS 292 From Gas to Stars over Cosmic Time Mordacai-Mark Mac Low (B) Tue. 21 IAUS 293 The Kepler Mission: NASA’s ExoEarth Census Natalie Batalha (3) Tue. 28 IAUS 294 The Origin and Evolution of Cosmic Magnetism Bryan Gaensler (B) Wed. 29 IAUS 295 Black Holes in Galaxies John Kormendy (B) Thu. 30 (c) Symposia - Week 1 IAUS 288 Astrophysics from Antartica IAUS 290 Accretion on all scales IAUS 291 Neutron Stars and Pulsars IAUS 292 Molecular gas, Dust, and Star Formation in Galaxies (d) Symposia –Week 2 IAUS 289 Advancing the Physics of Cosmic -
Istituto Di Radioastronomia Inaf
ISTITUTO DI RADIOASTRONOMIA INAF STATUS REPORT October 2007 http://www.ira.inaf.it/ Chapter 1. STRUCTURE AND ORGANIZATION The Istituto di Radioastronomia (IRA) is presently the only INAF structure with divisions distributed over the national territory. Such an organization came about because IRA was originally a part of the National Council of Research (CNR), which imposed the first of its own reforms in 2001. The transition from CNR to INAF began in 2004 and was completed on January 1st , 2005. The Institute has its headquarters in Bologna in the CNR campus area, and two divisions in Firenze and Noto. The Medicina station belongs to the Bologna headquarters. A fourth division is foreseen in Cagliari at the Sardinia Radiotelescope site. The IRA operates 3 radio telescopes: the Northern Cross Radio Telescope (Medicina), and two 32-m dishes (Medicina and Noto), which are used primarily for Very Long Baseline Interferometry (VLBI) observations. The IRA leads the construction of the Sardinia Radio Telescope (SRT), a 64-m dish of new design. This is one of the INAF large projects nowadays. The aims of the Institute comprise: - the pursuit of excellence in many research areas ranging from observational radio astronomy, both galactic and extragalactic, to cosmology, to geodesy and Earth studies; - the design and management of the Italian radio astronomical facilities; - the design and fabrication of instrumentation operating in bands from radio to infrared and visible. Main activities of the various sites include: Bologna: The headquarters are responsible for the institute management and act as interface with the INAF central headquarters in Roma. Much of the astronomical research is done in Bologna, with major areas in cosmology, extragalactic astrophysics, star formation and geodesy. -
A Decadal Strategy for Solar and Space Physics
Space Weather and the Next Solar and Space Physics Decadal Survey Daniel N. Baker, CU-Boulder NRC Staff: Arthur Charo, Study Director Abigail Sheffer, Associate Program Officer Decadal Survey Purpose & OSTP* Recommended Approach “Decadal Survey benefits: • Community-based documents offering consensus of science opportunities to retain US scientific leadership • Provides well-respected source for priorities & scientific motivations to agencies, OMB, OSTP, & Congress” “Most useful approach: • Frame discussion identifying key science questions – Focus on what to do, not what to build – Discuss science breadth & depth (e.g., impact on understanding fundamentals, related fields & interdisciplinary research) • Explain measurements & capabilities to answer questions • Discuss complementarity of initiatives, relative phasing, domestic & international context” *From “The Role of NRC Decadal Surveys in Prioritizing Federal Funding for Science & Technology,” Jon Morse, Office of Science & Technology Policy (OSTP), NRC Workshop on Decadal Surveys, November 14-16, 2006 2 Context The Sun to the Earth—and Beyond: A Decadal Research Strategy in Solar and Space Physics Summary Report (2002) Compendium of 5 Study Panel Reports (2003) First NRC Decadal Survey in Solar and Space Physics Community-led Integrated plan for the field Prioritized recommendations Sponsors: NASA, NSF, NOAA, DoD (AFOSR and ONR) 3 Decadal Survey Purpose & OSTP* Recommended Approach “Decadal Survey benefits: • Community-based documents offering consensus of science opportunities -
Solar Activity Affecting Space Weather
March 7, 2006, STP11, Rio de Janeiro, Brazil Solar Activity Affecting Space Weather Kazunari Shibata Kwasan and Hida Observatories Kyoto University, Japan contents • Introduction • Flares • Coronal Mass Ejections(CME) • Solar Wind • Future Projects Japanese newspaper reporting the big flare of Oct 28, 2003 and its impact on the Earth big flare (third largest flare in record) on Oct 28, 2003 X17 X-ray Intensity time A big flare on Oct 28, 2003 (third largest X-ray intensity in record) EUV Visible light SOHO/EIT SOHO/LASCO • Flare occurred at UT11:00 on Oct 28 Magnetic Storm on the Earth Around UT 6:00- Aurora observed in Japan on Oct 29, 2003 at around UT 14:00 on Oct 29, 2003 During CAWSES campaign observations (Shinohara) Xray X17 X6.2 Proton 10MeV 100MeV Vsw 44h 30h Bt Bz Dst Flares What is a flare ? Hα chromosphere 10,000 K Discovered in Mid 19C Near sunspots=> energy source is magnetic energy size~(1-10)x 104 km Total energy 1029 -1032erg (~ 105ー108 hydrogen bombs ) (Hida Observatory) Prominence eruption (biggest: June 4, 1946) Electro- magnetic Radio waves emitted from a flare (Svestka Visible 1976) UV 1hour time Solar corona observed in soft X-rays (Yohkoh) Soft X-ray telescope (1keV) Coronal plasma 2MK-10MK X-ray view of a flare Magnetic reconneciton Hα X-ray MHD simulation of a solar flare based on reconnection model including heat conduction and chromospheric evaporation (Yokoyama-Shibata 1998, 2001) A solar flare Observed with Yohkoh soft X-ray telescope (Tsuneta) Relation between filament (prominence) eruption and flare A flare -
Radio Spectroscopy of Stellar Flares: Magnetic Reconnection & CME
Solar and Stellar Flares and their Effects on Planets Proceedings IAU Symposium No. 320, 2015 c International Astronomical Union 2016 A.G. Kosovichev, S.L. Hawley & P. Heinzel, eds. doi:10.1017/S1743921316008644 Radio spectroscopy of stellar flares: magnetic reconnection & CME shocks in stellar coronae Jackie Villadsen1, Gregg Hallinan1 and Stephen Bourke1 1 Department of Astronomy, California Institute of Technology MC 249-17, 1200 E California Blvd, Pasadena, CA 91125, USA email: [email protected], [email protected], [email protected] Abstract. High-cadence spectroscopy of solar and stellar coherent radio bursts is a powerful diagnostic tool to study coronal conditions during magnetic reconnection in flares and to detect coronal mass ejections (CMEs). We present results from wide-bandwidth VLA observations of nearby active M dwarfs, including some observations with simultaneous VLBA imaging. We also discuss the Starburst program, which will make wide-bandwidth radio spectroscopic observations of nearby active flare stars for 20+ hours a day for multiple years, coming online in spring 2016 at the Owens Valley Radio Observatory. This program should vastly increase the diversity of observed stellar radio bursts and our understanding of their origins, and offers the potential to detect a population of CME-associated radio bursts. Keywords. stars: coronae, stars: flare, stars: individual (UV Ceti), stars: mass loss, Sun: coronal mass ejections (CMEs), Sun: radio radiation, radio continuum: stars 1. Introduction Many of the nearest habitable-zone Earths and super-Earths will be found around M dwarfs (Dressing & Charbonneau 2013). The magnetically active “youth” of M dwarfs lasts hundreds of millions to billions of years (West et al. -
GSFC Heliophysics Science Division 2009 Science Highlights
NASA/TM–2010–215854 GSFC Heliophysics Science Division 2009 Science Highlights Holly R. Gilbert, Keith T. Strong, Julia L.R. Saba, and Yvonne M. Strong, Editors December 2009 Front Cover Caption: Heliophysics image highlights from 2009. For details of these images, see the key on Page v. The NASA STI Program Offi ce … in Profi le Since its founding, NASA has been ded i cated to the • CONFERENCE PUBLICATION. Collected ad vancement of aeronautics and space science. The pa pers from scientifi c and technical conferences, NASA Sci en tifi c and Technical Information (STI) symposia, sem i nars, or other meetings spon sored Pro gram Offi ce plays a key part in helping NASA or co spon sored by NASA. maintain this impor tant role. • SPECIAL PUBLICATION. Scientifi c, techni cal, The NASA STI Program Offi ce is operated by or historical information from NASA pro grams, Langley Research Center, the lead center for projects, and mission, often concerned with sub- NASAʼs scientifi c and technical infor ma tion. The jects having substan tial public interest. NASA STI Program Offi ce pro vides ac cess to the NASA STI Database, the largest collec tion of • TECHNICAL TRANSLATION. En glish-language aero nau ti cal and space science STI in the world. trans la tions of foreign scien tifi c and techni cal ma- The Pro gram Offi ce is also NASAʼs in sti tu tion al terial pertinent to NASAʼs mis sion. mecha nism for dis sem i nat ing the results of its research and devel op ment activ i ties. -
NATIONAL ACADEMIES of SCIENCES and ENGINEERING NATIONAL RESEARCH COUNCIL of the UNITED STATES of AMERICA
NATIONAL ACADEMIES OF SCIENCES AND ENGINEERING NATIONAL RESEARCH COUNCIL of the UNITED STATES OF AMERICA UNITED STATES NATIONAL COMMITTEE International Union of Radio Science National Radio Science Meeting 4-8 January 2000 Sponsored by USNC/URSI University of Colorado Boulder, Colorado U.S.A. United States National Committee INTERNATIONAL UNION OF RADIO SCIENCE PROGRAM AND ABSTRACTS National Radio Science Meeting 4-8 January 2000 Sponsored by USNC/URSI NOTE: Programs and Abstracts of the USNC/URSI Meetings are available from: USNC/URSI National Academy of Sciences 2101 Constitution Avenue, N.W. Washington, DC 20418 at $5 for 1983-1999 meetings. The full papers are not published in any collected format; requests for them should be addressed to the authors who may have them published on their own initiative. Please note that these meetings are national. They are not organized by the International Union, nor are the programs available from the International Secretariat. ii MEMBERSHIP United States National Committee INTERNATIONAL UNION OF RADIO SCIENCE Chair: Gary Brown* Secretary & Chair-Elect: Umran S. !nan* Immediate Past Chair: Susan K. Avery* Members Representing Societies, Groups, and Institutes: American Astronomical Society Thomas G. Phillips American Geophysical Union Donald T. Farley American Meteorological Society vacant IEEE Antennas and Propagation Society Linda P.B. Katehi IEEE Geosciences and Remote Sensing Society Roger Lang IEEE Microwave Theory and Techniques Society Arthur A. Oliner Members-at-Large: Amalia Barrios J. Richard Fisher Melinda Picket-May Ronald Pogorzelski W. Ross Stone Richard Ziolkowski Chairs of the USNC/URSI Commissions: Commission A Moto Kanda Commission B Piergiorgio L. E. Uslenghi Commission C Alfred 0.