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Wednesday, May 13, 2020 | History

3 edition of Timing the Geminga pulsar with high-energy gamma-rays found in the catalog.

Timing the Geminga pulsar with high-energy gamma-rays

Timing the Geminga pulsar with high-energy gamma-rays

final technical report for NAG5-2051

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Published by National Aeronautics and Space Administration, Compton Gamma-Ray Observatory, National Technical Information Service, distributor in [Washington, DC?], [Springfield, Va .
Written in English

    Subjects:
  • Pulsars.,
  • Ephemerides.,
  • Gamma rays.,
  • Stellar rotation.,
  • Gamma ray astronomy.

  • Edition Notes

    Statementsubmitted by The Trustees of Columbia University ; prepared by Columbia Astrophysics Laboratory, Departments of Astronomy and Physics, Columbia University ; principal investigator, Jules P. Halpern.
    Series[NASA contractor report] -- NASA-CR-204445., NASA contractor report -- NASA CR-204445.
    ContributionsColumbia University. Trustees., Columbia Astrophysics Laboratory (Columbia University), Compton Observatory., United States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL15505764M

      Subjects: High Energy Astrophysical Phenomena (); High Energy Physics - Phenomenology (hep-ph) Gamma-ray bursts (GRBs) have been invoked to explain both the keV emission from the galactic bulge and the high-energy positron excess inferred from the ATIC, PAMELA, and Fermi data. While independent explanations can be responsible for. Algol is a triple system containing a 70 hr eclipsing binary (K IV and B8 V) in a day orbit with an A V star. The X-ray emission from this system (Schnopper et al ) is thought to be associated with a corona surrounding the lobe filling and synchron­ ously rotating K .

    The `rain’ of high-energy charged particles through the LAT (many thousands of particles per second) is much larger than the rate of celestial gamma rays (just a few per second), so the name of the game in gamma-ray astrophysics is background rejection — the detective work to identify the gamma rays. On the X-Ray and Infrared Enhancement of Anomalous X-ray Pulsar 1E + 20 minutes. M. Durant. Intrinsic spectra of magnetars: 20 minutes. P. R. den Hartog. AXP 4U + New INTEGRAL results and the first simultaneous multi-frequency observation campaign: 20 minutes. E. Gotthelf.

    Proceedings of the th Symposium of the International Astronomical Union held in Nanjing, China, May , The publication of this volume coincides with the 55th anni versary of the discovery of the neutron and Landau's suggestion at the time that one could make stars out of the new particles. This year also marks the twenty-fifth anniversary of the detection Book Edition: Beta particles are high-energy, high-speed electrons or positrons emitted by certain types of radioactive nuclei such as potassiumThe beta particles emitted are a form of ionizing radiation also known as beta rays. The production of beta particles is termed beta are designated by the Greek letter beta (β).. At right is a graph or block diagram that shows the .


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Timing the Geminga pulsar with high-energy gamma-rays Download PDF EPUB FB2

Get this from a library. Timing the Geminga pulsar with high-energy gamma-rays: final technical report for NAG [Jules P Halpern; Columbia University. Trustees.; Columbia Astrophysics Laboratory (Columbia University); Compton Observatory.; United States.

National Aeronautics and Space Administration.]. Timing The Geminga Pulsar With High Energy Gamma Rays Final Report Nasa Cr Jan 5 Author by: United States. National Aeronautics and Space Administration. Geminga / ɡ ə ˈ m ɪ ŋ ɡ ə / is a neutron star approximately parsecs (around light years) from the Sun in the constellation name, attributed by its discoverer Giovanni Bignami, is both a contraction of Gemini gamma-ray source, and a transcription of the words gh'è minga (pronounced [ɡɛ ˈmĩːɡa]), meaning "it's not there" in the Milanese dialect of llation: Gemini.

Presented here are recent VERITAS results from observational campaigns on the brightest northern-hemisphere high-energy gamma-ray pulsar Geminga and the missing link binary pulsar PSR J+ Author: Maxim Lyutikov. Geminga is the second brightest persistent source in the GeV gamma-ray sky.

Discovered in by SAS-2 mission, it was identified as a pulsar only in the 90s, when ROSAT detected the ms X-ray. The Fifth Compton Symposium, Portsmouth, NH, September byPortsmouth, NH> Compton Symposium. Book) Compton Observatory surveying the. If the address matches an existing account you will receive an email with instructions to reset your password.

However, the statistical significance of all the results is weak. In the end, Cygnus X-3 and similar object Hercules X-1 are not confirmed as emitters of TeV or PeV gamma rays, but the huge excitement from the putative detections greatly increases the interest in.

" Young ~ s emit from low-energy radio waves through high- energy X-rays and gamma rays. The radial lines emanating from a point show the relative distances to 14 ~ s from our Sun and the distance to the galactic core. This could conceivably be used by a clever species to identify our Sun's location within the Milky Way Galaxy.

Kuiper L, Hermsen W, Cusumano G, Diehl R, Schȯnfelder V, Strong A, Bennett K, McConnell ML () The Crab pulsar in the –30 MeV range as seen by CGRO COMPTEL. A coherent high-energy picture from soft X-rays up to high-energy gamma rays.

A&A Google Scholar. The universe is more than just stars, dust, and empty space. Explore some of the objects that make up our universe, from our own Sun to distant pulsars and black holes. Scientific discoveries often reveal new mysteries.

Take a look at a few of the mysteries that astronomers and astrophysicists are working on right now. Featured Science. Monthly Notices of the Royal Astronomical Society, ISSN7/, VolumeIssue 3, pp. - However, Geminga emits only gamma-ray pulses while B+54 is one of the brightest known radio pulsars, but emits no observable gamma rays.

@article{osti_, title = {Frequency dependence of pulsar integrated profiles}, author = {Thorsett, S E}, abstractNote = {The dependence of component separation on observing frequency has been studied for seven pulsars that exhibit double- or multiple-component average profiles.

In each case, a review of all available data shows a smooth variation of given form. The spacecraft's secondary instrument, the GBM, spotted 31 gamma-ray bursts in its first month of operation. These high-energy blasts occur when massive stars die and when orbiting neutron stars spiral together and merge.

The GBM is sensitive to lower energy range gamma rays ( to 30 million electronvolts) than LAT. Using the Tibet-III air shower array, we search for TeV {gamma}-rays from 27 potential Galactic sources in the early list of bright sources obtained by the Fermi Large Area Telescope at energies above MeV.

Among them, we observe seven sources instead of the expected sources at. Detectors for High-Energy Gamma-Rays: Functional Tests and Performance Characterization During the Assembly Phase of the Modules of the AGILE Silicon Tracker (M Basset et al.) Gamma Air Watch (GAW) — An Imaging Atmospheric Cherenkov Telescope Large with Large Field of View (T Mineo et al.).

The pulsar is named Geminga, and it’s one of the nearest pulsars to Earth, about light years away in the constellation Gemini. Not only is. The likely detection of pulsed high-energy gamma-ray emission from millisecond pulsar PSR J + Astronomy and Astrophysics,– ADS Google ScholarCited by: 7.

- Explore wbacon's board "Pulsars", followed by people on Pinterest. See more ideas about Neutron star, Astronomy and Astrophysics pins. First Detection of an X-Ray Burst and a One Hour Intensity Dip in 4U Detection of Iron Lines in the Persistent Emission of Some X-Ray Burst Sources Observed by EXOSAT.- The Variable Iron Line in Cygnus X Long Term Observations of Cyg X-3 with Vela 5B.- Cyg X-3 Not Seen at High-Energy Gamma Rays.-Author: A.

Peacock.Among this set of candidate sources we found that only the Monogem (PSR B+14) at a distance of d = p c and age T = × 10 5 y e a r s (Manchester et al. ), and the Geminga pulsar (PSR J+) with d = p c and T = × 10 5 y e a r s (Caraveo et al. Caraveo) give a significant contribution to the high energy Cited by: HIGH ENERGY GAMMA-RAY ASTRONOMY: 5th International Meeting on High Energy Gamma-Ray Astronomy.

AIP Conference Proceedings, Volume .