Toward an Understanding of the Progenitors of Gamma-Ray Bursts
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On the Association of Gamma-Ray Bursts with Supernovae Dieter H
Clemson University TigerPrints Publications Physics and Astronomy Summer 7-24-1998 On the Association of Gamma-Ray Bursts with Supernovae Dieter H. Hartmann Department of Physics and Astronomy, Clemson University, [email protected] R. M. Kippen Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville & NASA/Marshall Space Flight Center & NASA/Marshall Space Flight Center M. S. Briggs Physics Department, University of Alabama in Huntsville & NASA/Marshall Space Flight Center J. M. Kommers Department of Physics and Center for Space Research, Massachusetts nI stitute of Technology C. Kouveliotou Universities Space Research Association & NASA/Marshall Space Flight Center See next page for additional authors Follow this and additional works at: https://tigerprints.clemson.edu/physastro_pubs Recommended Citation Please use publisher's recommended citation. This Article is brought to you for free and open access by the Physics and Astronomy at TigerPrints. It has been accepted for inclusion in Publications by an authorized administrator of TigerPrints. For more information, please contact [email protected]. Authors Dieter H. Hartmann, R. M. Kippen, M. S. Briggs, J. M. Kommers, C. Kouveliotou, K. Hurley, C. R. Robinson, J. van Paradijs, T. J. Galama, and P. M. Vresswijk This article is available at TigerPrints: https://tigerprints.clemson.edu/physastro_pubs/83 Re-Submitted to ApJL 24-Jul-98 On the Association of Gamma-Ray Bursts with Supernovae R. M. Kippen,1,2,3 M. S. Briggs,4,2 J. M. Kommers,5 C. Kouveliotou,6,2 K. Hurley,7 C. R. Robinson,6,2 J. van Paradijs,5,8 D. H. Hartmann,9 T. -
Physical Parameters of GRB 970508 and GRB 971214 from Their
SUBMITTED 22-APR-99 TO ASTROPHYSICAL JOURNAL, IN ORIGNAL FORM 26-MAY-98 Preprint typeset using LATEX style emulateapj PHYSICAL PARAMETERS OF GRB 970508 AND GRB 971214 FROM THEIR AFTERGLOW SYNCHROTRON EMISSION R.A.M.J. WIJERS1 AND T.J. GALAMA2 SUBMITTED 22-APR-99 to Astrophysical Journal, in orignal form 26-MAY-98 ABSTRACT We have calculated synchrotron spectra of relativistic blast waves, and find predicted characteristic frequencies that are more than an order of magnitude different from previous calculations. For the case of an adiabatically expanding blast wave, which is applicable to observed gamma-ray burst (GRB) afterglows at late times, we give expressions to infer the physical properties of the afterglow from the measured spectral features. We show that enough data exist for GRB970508to compute unambiguously the ambient density, n =0.03cm−3, and the blast wave energy per unit solid angle, =3 1052 erg/4π sr. We also compute the energy density in electrons and magnetic field. We find that they areE 12%× and 9%, respectively, of the nucleon energy density and thus confirm for the first time that both are close to but below equipartition. For GRB971214,we discuss the break found in its spectrum by Ramaprakash et al. (1998). It can be interpreted either as the peak frequency or as the cooling frequency; both interpretations have some problems, but on balance the break is more likely to be the cooling frequency. Even when we assume this, our ignorance of the self- absorption frequency and presence or absence of beaming make it impossible to constrain the physical parameters of GRB971214 very well. -
What Is CHEOPS?
Swiss and ESA satellite CHEOPS launching soon! CHEOPS will be launching into space on the 17th of December! You may be wondering: what is CHEOPS? CHEOPS stands for CHaracterising ExOPlanet Satellite. Its goal is to study transits of already-known exoplanets to gain more knowledge about them. What type of information are we looking for? Scientists want to know detailed information about planets outside our Solar System, such as the mass, planet size, and density, which will in turn help to figure out the composition of these exoplanets. Studying exoplanet composition and their atmospheres is important especially for astrobiology. A planet’s chemical composition can affect its habitability for life as we know it. Scientists usually look for biosignatures such as the presence of methane or oxygen in the planet’s atmosphere, which could indicate presence of past or present life. Artist’s impression of CHEOPS. Credits: ESA / ATG medialab. The major contributors CHEOPS is a collaboration between ESA and the Swiss Space Office. The mission was proposed and is now headed by Prof. Willy Benz, from the University of Bern, which houses the mission’s consortium. The science operations consortium is at the University of Geneva, where they have many collaborators, such as the Swiss Space Center at EPFL. As it is an ESA endeavour, many other European institutions are also contributing to the mission. For example, the mission operations consortium is located in Torrejón de Ardoz, Spain. The launch The satellite has already been shipped to Kourou, French Guiana, where it will be launched by the ESA spaceport. -
Exoplanet Tool Kit
Exoplanet Tool Kit New Mexico Super Computing Challenge Final Report April 5, 2011 Team 35 Desert Academy Team Members Chris Brown Isaac Fischer Teacher Jocelyn Comstock Mentors Henry Brown Prakash Bhakta Table of Contents Executive Summary ................................................................................................ 2 Background ............................................................................................................ 3 Astrophysics .............................................................................................. 3 Definition and Origin of Extroplanets ....................................................... 4 Methods of Detection ............................................................................... 4 Project .................................................................................................................. 6 Methodology............................................................................................. 6 Data Results .............................................................................................. 7 Conclusion ............................................................................................................ 10 Future Study ......................................................................................................... 11 Acknowledgements.............................................................................................. 12 References .......................................................................................................... -
NL#135 May/June
May/June 2007 Issue 135 A Publication for the members of the American Astronomical Society 3 IOP to Publish President’s Column AAS Journals J. Craig Wheeler, [email protected] Whew! A lot has happened! 5 Member Deaths First, my congratulations to John Huchra who was elected to be the next President of the Society. John will formally become President-Elect at the meeting in Hawaii. He will then take over as President at the meeting in St. Louis in June of 2008 and I will serve as Past-President until the 6 Pasadena meeting in June of 2009. We have hired a consultant to lead a one-day Council retreat before the Hawaii meeting to guide the Council toward a more strategic outlook for the Society. Seattle Meeting John has generously agreed to join that effort. I know he will put his energy, intellect, and experience Highlights behind the health and future of the Society. We had a short, intense, and very professional process to issue a Request for Proposals (RFP) to 10 publish the Astrophysical Journal and the Astronomical Journal, to evaluate the proposals, and Award Winners to select a vendor. We are very pleased that the IOP Publishing will be the new publisher of our cherished and prestigious journals and are very optimistic that our new partnership will lead to in Seattle a necessary and valuable evolution of what it means to publish science journals in the globally- connected electronic age. 11 The complex RFP defining our journals and our aspirations for them was put together by a team International consisting of AAS representatives and outside independent consultants. -
The Search for Planets Around Other Stars by Andrew Fraknoi, Astronomical Society of the Pacific
www.astrosociety.org/uitc No. 19 - Winter 1991-92 © 1992, Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, CA 94112 The Search for Planets Around Other Stars by Andrew Fraknoi, Astronomical Society of the Pacific The question of whether there are planets outside our Solar System has intrigued scientists, science fiction writers and poets for years. But how can we know if any really exist? We devote this issue of The Universe in the Classroom to the search for planets around other stars. What is the difference between a planet and a star? Why do we think there might be planets around other stars? Why is it so hard to see planets around other stars? If we can't see them, how can we find out if there are planets around other stars? Have any planets been detected from stellar wobbles? The Case of Barnard's Star Are there other ways to detect planets? Can we see the large disks of gas and dust around other stars out of which planets form? What about reports of planets around pulsars? Activity: Center of Mass Demonstration What is the difference between a planet and a star? Stars are huge luminous balls of gas powered by nuclear reactions at their centers. The enormously high temperatures and pressures in the core of a star force atoms of hydrogen to fuse together and become helium atoms, releasing tremendous amounts of energy in the process. Planets are much smaller with core temperatures and pressures too low for nuclear fusion to occur. Thus they emit no light of their own. -
Monte Carlo Simulations of GRB Afterglows
ABSTRACT WARREN III, DONALD CAMERON. Monte Carlo Simulations of Efficient Shock Acceleration during the Afterglow Phase of Gamma-Ray Bursts. (Under the direction of Donald Ellison.) Gamma-ray bursts (GRBs) signal the violent death of massive stars, and are the brightest ex- plosions in the Universe since the Big Bang itself. Their afterglows are relics of the phenomenal amounts of energy released in the blast, and are visible from radio to X-ray wavelengths up to years after the event. The relativistic jet that is responsible for the GRB drives a strong shock into the circumburst medium that gives rise to the afterglow. The afterglows are thus intimately related to the GRB and its mechanism of origin, so studying the afterglow can offer a great deal of insight into the physics of these extraordinary objects. Afterglows are studied using their photon emission, which cannot be understood without a model for how they generate cosmic rays (CRs)—subatomic particles at energies much higher than the local plasma temperature. The current leading mechanism for converting the bulk energy of shock fronts into energetic particles is diffusive shock acceleration (DSA), in which charged particles gain energy by randomly scattering back and forth across the shock many times. DSA is well-understood in the non-relativistic case—where the shock speed is much lower than the speed of light—and thoroughly-studied (but with greater difficulty) in the relativistic case. At both limits of speed, DSA can be extremely efficient, placing significant amounts of energy into CRs. This must, in turn, affect the structure of the shock, as the presence of the CRs upstream of the shock acts to modify the incoming plasma flow. -
Who Really Discovered the First Exoplanet?
Who Really Discovered the First Exoplanet? Two Swiss astronomers got a well-deserved Nobel for finding an exoplanet, but there’s an intriguing backstory By Josh Winn The year 1995, like 1492, was the dawn of an age of discovery. The new explorers, instead of using seagoing vessels to discover continents, use telescopes to discover planets revolving around distant stars. Thousands of these extrasolar planets, a term usually shortened to “exoplanets,” have been found, including a few potentially Earth- like worlds, along with bizarre objects that bear no resemblance to any of the planets in our solar system. Two of these exoplanet explorers, Michel Mayor and Didier Queloz, were recently awarded half of the Nobel Prize in Physics for the discovery they made in 1995. My colleagues and I are united in our admiration for their pioneering work, and in our pride to be continuing what they began. But there is something peculiar about the Nobel Prize citation. It says: “for the discovery of an exoplanet orbiting a solar-type star.” Shouldn’t it say the first exoplanet? After all, hundreds of astronomers have discovered an exoplanet. I’ve helped find a few. Even high school students and amateur astronomers have discovered them. Did the Nobel Committee make a typographical error? No, they did not, and thereby hangs a tale. Just as it is problematic to decide who discovered America (Christopher Columbus? John Cabot? Leif Erikson? Amerigo Vespucci, whose name is the one that stuck? Those who came on foot from Siberia tens of thousands of years ago?) it is difficult to say who discovered the first exoplanet. -
Theory of Gamma-Ray Burst Emission in Light of BSAX Results
1 Theory of Gamma-Ray Burst Emission in Light of BSAX Results⋆ M. Tavani a,b a IFCTR/CNR, via Bassini 15, I-20133 Milano (Italy). b Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027 (USA). We briefly discuss the theoretical implications of recent detections of gamma-ray bursts (GRBs) by BSAX. Relativistic shock wave theories of fireball expansion are challenged by the wealth of X-ray, optical and radio data obtained after the discovery of the first X-ray GRB afterglow. BSAX data contribute to address several issues concerning the initial and afterglow GRB emission. The observations also raise many questions that are still unsolved. The synchrotron shock model is in very good agreement with time-resolved broad-band spectra (2–500 keV) for the majority of GRBs detected by BSAX. 1. A Year of Surprise optical and radio data, and many problems re- main unsolved at the moment. We briefly discuss The discovery of X-ray afterglows by BSAX here some of the open issues. revolutionized the field of GRB research [8,14, BSAX showed for the first time that a sub- 35]. The discovery cought us by surprise. Cer- stantial fraction of GRB energy is dissipated in tainly, there was no theoretical prediction of hard the X-ray range at late times (hours, days, some- [14,51] high-energy emission lasting hours-days times weeks) after the main impulsive events. after the main events. ‘Pre-BSAX models’ of Are classical GRBs the tip of the iceberg of more GRB shock waves predicted a much faster decay complex radiation processes lasting much longer of the hard component produced by the initial than expected from the cooling timescales of ini- impulsive particle acceleration (e.g., [25]). -
Constraining the Beaming of Gamma- Ray Bursts with Radio Surveys
Constraining the Beaming of Gamma- Ray Bursts with Radio Surveys The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Perna, Rosalba, and Abraham Loeb. 1998. “Constraining the Beaming of Gamma-Ray Bursts with Radio Surveys.” The Astrophysical Journal 509 (2): L85–88. https:// doi.org/10.1086/311784. Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:41393210 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Other Posted Material, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#LAA The Astrophysical Journal, 509:L85±L88, 1998 December 20 q 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. CONSTRAINING THE BEAMING OF GAMMA-RAY BURSTS WITH RADIO SURVEYS Rosalba Perna and Abraham Loeb Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 Received 1998 October 6; accepted 1998 October 22; published 1998 November 10 ABSTRACT The degree of beaming in gamma-ray bursts (GRBs) is currently unknown. The uncertainty in the g-ray±beaming / 2 / 22 angle, vb, leaves the total energy release (vbb ) and the event rate per galaxy (v ) unknown to within orders of magnitude. Since the delayed radio emission of GRB sources originates from a mildly relativistic shock and receives only weak relativistic beaming, the rate of radio-selected transients with no GRB counterparts can be 22 » used to set an upper limit onvb . We ®nd that a VLA survey with a sensitivity of 0.1 mJy at 10 GHz could * # 4 C 22 identify 2 10 (vb /10 ) radio afterglows across the sky if each source is sampled at least twice over a period of 1 month or longer. -
Introduction
Cambridge University Press 0521828236 - Handbook of Pulsar Astronomy D. R. Lorimer and M. Kramer Excerpt More information Introduction Radio pulsars – rapidly rotating highly magnetised neutron stars – are fascinating objects to study. Weighing more than our Sun, yet only 20 km in diameter, these incredibly dense objects produce radio beams that sweep the sky like a lighthouse. Since their discovery by Jocelyn Bell- Burnell and Antony Hewish at Cambridge in 1967 (Hewish et al. 1968), over 1600 have been found. Pulsars provide a wealth of information about neutron star physics, general relativity, the Galactic gravitational potential and magnetic field, the interstellar medium, celestial mechan- ics, planetary physics and even cosmology. Milestones of radio pulsar astronomy Pulsar research has been driven by numerous surveys with large ra- dio telescopes over the years. As well as improving the overall census of neutron stars, these searches have discovered exciting new objects, e.g. pulsars in binary systems. Often, the new discoveries have driven designs for further surveys and detection techniques to maximise the use of available resources. The landmark discoveries so far are: • The Cambridge discovery of pulsars (Hewish et al. 1968). Hewish’s contributions to radio astronomy, including this discovery, were recog- nised later with his co-receipt of the 1974 Nobel Prize for Physics with Martin Ryle. • The first binary pulsar B1913+161 by Russell Hulse and Joseph Taylor at Arecibo in 1974 (Hulse & Taylor 1975). This pair of neutron stars 1 Pulsars are named with a PSR prefix followed by a ‘B’ or a ‘J’ and their celestial coordinates. Pulsars discovered before 1990 usually are referred to by their ‘B’ names (Besselian system, epoch 1950). -
A Relativistic Particle Outburst from the Soft Gamma-Ray Repeater SGR1900+ 14
A relativistic particle outburst from the soft gamma-ray repeater 1900+14 D. A. Frail1, S. R. Kulkarni2 & J. S. Bloom2 1National Radio Astronomy Observatory, P. O. Box 0, Socorro, NM 87801, USA 2California Institute of Technology, Owens Valley Radio Observatory 105-24, Pasadena, CA 91125, USA Abstract. Soft gamma-ray repeaters (SGR) are a class of high energy transients whose brief emissions are thought to arise from young1 and highly magnetized neutron stars2,3,4,5,6. The exact cause for these outbursts and the nature of the energy loss remain unknown. Here we report the discovery of a fading radio source within the localization of the relatively under-studied SGR 1900+14. We argue that this radio source is a short-lived nebula powered by the parti- cles ejected during the intense high energy activity in late August 1998, which included the spectacular gamma-ray burst7 of August 27. The radio observa- tions allow us to constrain the energy released in the form of particles ejected during the burst, un-complicated by beaming effects. Furthermore, thanks to the astrometric precision of radio observations, we have finally localized this repeater to sub-arcsecond accuracy. This manuscript has been submitted to Nature on 27 October, 1998. For further enquiries please contact Dale Frail ([email protected]) or Shri Kulkarni ([email protected]). arXiv:astro-ph/9812457v1 28 Dec 1998 –1– Until recently SGR 1900+14 was routinely labeled as the least prolific of the SGRs with only three bursts8 in 1979 and another three9 in 1992. We investigated the relatively crude localization obtained from the 1979 activity and suggested10 that this SGR is asso- ciated with the supernova remnant (SNR) G 42.8+0.6 (see also ref.