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Wednesday, October 21, 2020 | History

3 edition of X-ray flare characteristics in lambda Eridani (ROSAT) found in the catalog.

X-ray flare characteristics in lambda Eridani (ROSAT)

X-ray flare characteristics in lambda Eridani (ROSAT)

final report for NASA contract S-57776-F

  • 106 Want to read
  • 25 Currently reading

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

    Subjects:
  • B stars.,
  • Variable stars.,
  • X rays.,
  • Stellar flares.

  • Edition Notes

    StatementMyron A. Smith.
    Series[NASA contractor report] -- NASA-CR-204076., NASA contractor report -- NASA CR-204076.
    ContributionsUnited States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL18131616M

      Ngôi sao cháy gần Những ngôi sao cháy thực chất mờ nhạt, nhưng đã được tìm thấy ở khoảng cách năm ánh sáng từ Trái đất. Vào ngày 23 tháng 4 năm , vệ tinh Swift của NASA đã phát hiện ra chuỗi pháo sáng mạnh nhất, nóng nhất và kéo dài nhất từng thấy từ một sao lùn đỏ gần :// ‘The third edition of Malcolm Longair’s High Energy Astrophysics is a remarkable gem. It is written in the clear, lucid style that characterizes Professor Longair’s monographs and displays an admirable balance between breadth and ://

    Fermi/LAT bright gamma-ray source list (0FGL) (Abdo+, ) (J/ApJS//46) () 10C survey of radio sources at GHz (Davies+, ) (J/MNRAS//() The Parkes quarter-Jansky flat-spectrum sample (Jackson+, ) (J/A+A//97() Star formation in spectroscopic survey (Carter+, ) (J/ApJ//() Counts and spectral indices at GHz (Windhorst+, ) (J/ApJ//   A pulsar (short for pulsating radio star) is a highly magnetized, rotating neutron star that emits a beam of electromagnetic radiation can be observed only when the beam of emission is pointing toward Earth, much the way a lighthouse can be seen only when the light is pointed in the direction of an observer, and is responsible for the pulsed appearance of ://

    This X-ray flare is similar to the X-ray flaring seen at a similar orbital phase in previous binary orbital cycles. X-ray flaring should continue until the star reaches it X-ray maximum before the decline to the X-ray minimum on February Viewing tool updated (02 Dec ) Support for the upcoming IXPE mission has been added to ://   The flare activity associated with Proxima, in which the X-ray luminosity can vary by factors of order 10 to on a timescale of minutes (Güedel. ), will presumably have a profound effect upon the habitability of any associated planet(s), even if they do orbit within its canonical HZ (Odert.


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X-ray flare characteristics in lambda Eridani (ROSAT) Download PDF EPUB FB2

Microfiche. [Washington, D.C.: National Aeronautics and Space Administration, ]. 1 microfiche. Header title: X-ray flare characteristics in the B2e star Lambda Eridani.

Description: 1 volume. X-ray flare characteristics in lambda Eridani book Title: NASA contractor report, NASA CR Other Titles: X-ray flare characteristics in the B2e star Lambda Eridani: Responsibility: Myron Title: X-Ray Flare Characteristics in Lambda Eridani: Authors: Smith, Myron A.

Affiliation: AA(Computer Sciences Corp.) Publication: Technical Report, Computer Sciences Corp. Calverton, MD United Final report for on task (SP) entitled "X-ray flare characteristics in lambda Eridani" X-Ray Flare Characteristics in lambda Eridani. By Myron A. Smith. Abstract.

The X-ray component consisted of observations from both the ASCA and ROSAT satellites Topics: Space Radiation. Year: OAI identifier: oai:   X-ray flaring from ROSAT observations in The X-ray component consisted of observations from both ROSAT (subject of this task) and ASCA satellites.

The flare event observed by ROSAT caught the astronomical hot star community by surprise because X-ray flares have not been observed from other single B-type stars, before or :// A giant X-ray flare on Lambda Eridani (B2e) Authors: Smith, Myron A.;can be fitted well to a Raymond-Smith temperature parameter of 14 MK and luminosity 4 x 10 exp 31 ergs/s; these are characteristics of giant stellar flares.

With an estimated duration of ab s, this event is arguably the strongest X-ray flare yet observed LS. Final Report for on Task (SP) entitled: "X-Ray Flare Characteristics in lambda Eridani" (ASCA) Myron A.

Smith, CSC/Science Programs This proposal was for a joint X-rayultravioletground-based study of the abnormal Be star lambda Eri, which has previously shown evidence of X-ray flaring from ROSAT observations in Artificial intelligence in clinical research.

X-Ray Flare Characteristics in the B2e Star Lambda Eridani (ROSAT) April /_Artificial_intelligence_in_clinical_research. STARS and STARS OF THE WEEK Star Count: Created by Jim Kaler, Prof. Emeritus of Astronomy, University of Illinois Learn about stellar spectra in STARS AND THEIR SPECTRA: An Introduction to the Spectral Sequence, Second Ed., with two new chapters and new illustrations, Cambridge University Press (UK or North America), From the Sun to the Stars: the OLLI   Uma estrela eruptiva é uma estrela variável que pode passar por aumentos dramáticos e imprevisíveis no seu brilho por alguns minutos.

Acredita-se que, assim como as erupções solares, as dessas estrelas se devam à energia magnética armazenada na atmosfera das mesmas. O aumento de brilho ocorre, no espectro eletromagnético, desde raios-X até ondas de :// X-Ray Flare Characteristics in the B2e Star Lambda Eridani (ROSAT) We have made three ROSAT HRI observations of the Orion Nebula region, ranging in exposure time from ~ 10 to ~ 50 ksecs.

/_ROSAT_HRI_Observations_of_the_Orion_Nebula. Within the Multimedia Gallery section you will find sets of images relating to: Scientific results (real images, artistic representations, animations, etc.). Institutional events (meetings, educational activities, etc.).

Facilities and instrumentation of the IAC and the Observatorios de Canarias;   Bibliography Myron Smith Buta, R.

and Smith, M. "The Light Variations of Nonradial Pulsations. Theory and Application to Line Profile Variations ~msmith/ "Discovery of a variable supersoft X-ray source in the Large Magellanic Cloud during the ROSAT All-Sky Survey," Astronomy and Astrophysics, L9-L Schelgel, E.M.; Petre, R.; July "A ROSAT upper limit on X-ray emission from SN A," Astrophysical Journal, Part 2 - Letters,1, LL   Occasionally, a star passing too near an MBH is torn apart by gravitational forces, leading to a bright tidal disruption flare (TDF).

Although the hi PMID X-ray Astrophysical X-ray spectroscopy promises huge potential scientific returns. The soft X-ray bandpass, keV, contains transitions from the K- L- and M-shell of every cosmically abundant element and ion except H and He. With only moderate (R ~ ) resolution, these transitions can be separated into gas, molecular, and solid state :// Instability and Variability of Hot-Star Winds Proceedings of an International Workshop Held at Isle-aux-Coudres, Quebec Province, Canada 23–27 August, Buy Physical Book Learn about institutional subscriptions.

Papers Table of Constraints on Hot Star X-Ray Source Characteristics from Combined Analysis of X-Ray and UV Observations   Serpens ("the Serpent", Greek Ὄφις) is a constellation of the northern of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent Head) to the west In the search for life beyond Earth, astronomers look for planets in a star's "habitable zone" — sometimes nicknamed the "Goldilocks zone" — where temperatures are just right for liquid water to exist on a planet's surface.

But, what kinds of stars might be best for life. Effects of Proxima Centauri on Planet Formation in Alpha Centauri WORTH R. & SIGURDSSON S. ApJ,paper arxiv ADS Optical, UV, and X-Ray Evidence for.

Coronal astronomy is by now a fairly mature discipline, with a quarter century having gone by since the detection of the first stellar X-ray coronal source (Capella), and having benefitted from a series of major orbiting observing facilities. Serveral observational characteristics of coronal X-ray and EUV emission have been solidly established through extensive observations, and are by now :SPACProc.

SPIE.EUV and X-ray Optics: Synergy between Laboratory and Space VI  Helium Line Emissions from the Outer Atmosphere of lambda Eridani",Ap.J,Smith, J"Chandra Detection of an X-Ray Flare from the Brown Dwarf LP ","Characteristics of Planetary Candidates Observed by Kepler.

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