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3 edition of [ROSAT observations of the binary BE-star/radio pulsar PSR1259-6] found in the catalog.

[ROSAT observations of the binary BE-star/radio pulsar PSR1259-6]

[ROSAT observations of the binary BE-star/radio pulsar PSR1259-6]

[semiannual technical report, 15 Jan. - 1 Aug. 1993]

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • Pulsars.

  • Edition Notes

    Statementprepared by Lynn R. Cominsky, principal investigator.
    SeriesNASA contractor report -- NASA CR-194394.
    ContributionsUnited States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL17680415M

    Other articles where Binary pulsar is discussed: Arecibo Observatory: Arecibo to discover the first binary pulsar. They showed that it was losing energy through gravitational radiation at the rate predicted by physicist Albert Einstein’s theory of general relativity, and they won the Nobel Prize for Physics in for their discovery. PSR J− is the only known double consists of two neutron stars emitting electromagnetic waves in the radio wavelength in a relativistic binary two pulsars are known as PSR J−A and PSR J−B. It was discovered in at Australia's Parkes Observatory by an international team led by the radio astronomer Marta Burgay during a high-latitude pulsar.

    Voyager's Golden Record is a inch gold-plated copper disk, encoded with music, sounds and images from Earth. Its aluminum cover is engraved with instructions, and a unique galactic map. PSR JA is a binary pulsar with a helium white dwarf (HeWD) companion located about 6 arcmin from the center of the globular cluster NGC Based on 12 years of observations at the Parkes radio telescope, the relativistic Shapiro delay has been detected in this system. We obtain a companion mass M{sub C} = {+-} M {sub Sun.

      In the binary system, the pulsar and its companion star orbit the the common center of mass in only hours. The companion is heated on one side by the pulsar's radiation (magenta) and is slowly.   A pulsar is a type of neutron star that must be both magnetized and moving very fast, because it spins its magnetic field fast enough to .


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[ROSAT observations of the binary BE-star/radio pulsar PSR1259-6] Download PDF EPUB FB2

"ROSAT Observations of the Binary Be-star/Radio Pulsar PSR", Dr. Lynn R. Cominsky, Principal Investigator, Department of Physics and Astronomy, Sonoma State University, Rohnert Park, CA   Get this from a library. [ROSAT observations of the binary BE-star/radio pulsar PSR]: [semiannual technical report, 15 Jan.

- 1 Aug. [Lynn R Cominsky; United States. [ROSAT observations of the binary BE-star/radio pulsar PSR1259-6] book National Aeronautics and Space Administration.].

Get this from a library. ROSAT observations of the binary Be-star/radio pulsar PSR final technical report for NASA NAG [Lynn R Cominsky; United States.

National Aeronautics and Space Administration.]. We report on results of X-ray observations of the unique radio pulsar/Be star binary PSR B - 63, obtained using the ASCA satellite 2 weeks before, during, and 2 weeks after the pulsar. [ROSAT observations of the binary BE-star/radio pulsar PSR] [microform]: [semiannual technical re [High time resolution studies of binary X ray pulsars] [microform]: [semiannual technical report, 1 Sep Pulsars / Richard N.

Manchester, Joseph H. Taylor; Clocks in the sky: the story of pulsars / Geoff McNamara; Pulsars / F. Smith. Radio pulsars with millisecond spin periods are thought to have been spun up by the transfer of matter and angular momentum from a low-mass companion star during an x-ray–emitting phase.

The spin periods of the neutron stars in several such low-mass x-ray binary (LMXB) systems have been shown to be in the millisecond regime, but no radio pulsations.

The Relativistic Binary Pulsar B+ Thirty Years of Observations and Analysis: Weisberg, J.M.; Taylor, J.H. Timing the Relativistic Binary Pulsar PSR J Bailes, M. Binary Pulsar Discoveries in the Parkes Multibeam Survey: Lyne, A.G.

New Binary and Millisecond Pulsars from Arecibo Drift-Scan Searches: The observations around the periastron passage of the pulsar were performed with the four 13m Cherenkov telescopes of the H.E.S.S.

experiment, recently installed in Namibia and in full operation since December Between February and Junea γ-ray signal from the binary system was detected with a total significance above 13 σ. Deep R band CCD photographs of the region surrounding the binary pulsar PSR + 16 have been obtained with the 4-m telescope of the Kitt Peak National Observatory.

Using an. Available in the National Library of Australia collection. Author: Graham-Smith, Francis, Sir, ; Format: Book; xii, pages: illustrations ; 24 cm. The thick lines show the periods as measured during GBT observations. Bottom: Similar Doppler variations from the highly eccentric binary MSP JA in the globular cluster NGC This pulsar has one of the most eccentric orbits known (e = ) and a massive white-dwarf or neutron-star companion.

The Relativistic Binary Pulsar B+ Thirty Years of Observations and Analysis: Volume:Binary Radio Pulsars: Page: Authors: Weisberg, J.M.; Taylor, J.H. Abstract: We describe results derived from thirty years of observations of PSR B+ Together with the Keplerian orbital parameters, measurements of the relativistic.

the binary radio pulsar population and proposed the existence of an as yet unidenti ed class of binary pulsars. Second, we conducted an in-depth analysis of the eclipses in. Radio pulsars with millisecond spin periods are thought to have been spun up by the transfer of matter and angular momentum from a low-mass companion star during an x-ray-emitting phase.

The spin periods of the neutron stars in several such low-mass x-ray binary (LMXB) systems have been shown to be in the millisecond regime, but no radio pulsations have been detected.

Binary Pulsars as a Test of General Relativity. A pulsar is a rotating neutron star that produces periodic signals in Earth detectors as its beam of radiation sweeps over Earth once per rotation. A binary pulsar may have the additional feature of a measurable decrease in the orbital period as the two pulsars spiral inward toward each other.

This change in the orbital period can be. Confirmatory observations made in Marchshowed a variable pulse frequency indicating a Doppler shift due to a periodic orbit around another object 6. A compilation of measured system. [ROSAT observations of the binary BE-star/radio pulsar PSR].

[Washington, DC Springfield, Va. Cominsky, Lynn, Mallory Roberts, Mark Finger and United States. National Aeronautics and Space Administration. April outburst from 4U+63 observed by BATSE. [Washington, DC Springfield, Va. Cominsky, L. A binary pulsar is a pulsar with a binary companion, often a white dwarf or neutron star.

(In at least one case, the double pulsar PSR J, the companion neutron star is another pulsar as well.)Binary pulsars are one of the few objects which allow physicists to test general relativity because of the strong gravitational fields in their vicinities.

NC 08/ A COMINSKY, L. ROSAT observations of the binary Be-star/radio pulsar PSR NV 07/ A VANGORKOM, J. ROSAT: X ray survey of compact groups. The metallic and Hα radial velocity semi-amplitude determined from the pulsar-state observations allows us to constrain the secondary star’s true radial velocity K 2 = ± km s −1 and the binary mass ratio q = ± By comparing the observed metallic and Hα absorption-line radial velocity semi-amplitudes with model.

Hence, if general relativity is correct then the observed value (dP dt) O of the variation in orbital period of the pulsar provides an upper bound for dE′ dt given as (4) dE′ dt ≤ πG 5/3 5c 5 P 2π −5/3 f(e)M p M c M −1/3 − dP dt O 1 3 (2πGM) 2/3 μP −5/3, where P is the orbital period of the pulsar.The pulsar/massive star binary system PSR B/LS is one of the best-studied gamma-ray binaries, a class of systems whose bright gamma-ray flaring can provide important insights into high-energy physics.

Using the Australian Long Baseline Array, we have conducted very long baseline interferometric observations of PSR B over years, fully .Abstract. PSR J− is a young pulsar in orbit around a companion that is most likely a B-type main-sequence star.

Since its discovery more than a decade ago, data have been taken at several frequencies with instruments at the Green Bank.