X-ray flare characteristics in lambda Eridani (ROSAT)

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. Series 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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