Search Results - (Author, Cooperation:S. M. Kahn)
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1Latest Papers from Table of Contents or Articles in PressS. Bernitt ; G. V. Brown ; J. K. Rudolph ; R. Steinbrugge ; A. Graf ; M. Leutenegger ; S. W. Epp ; S. Eberle ; K. Kubicek ; V. Mackel ; M. C. Simon ; E. Trabert ; E. W. Magee ; C. Beilmann ; N. Hell ; S. Schippers ; A. Muller ; S. M. Kahn ; A. Surzhykov ; Z. Harman ; C. H. Keitel ; J. Clementson ; F. S. Porter ; W. Schlotter ; J. J. Turner ; J. Ullrich ; P. Beiersdorfer ; J. R. Lopez-Urrutia
Nature Publishing Group (NPG)
Published 2012Staff ViewPublication Date: 2012-12-14Publisher: Nature Publishing Group (NPG)Print ISSN: 0028-0836Electronic ISSN: 1476-4687Topics: BiologyChemistry and PharmacologyMedicineNatural Sciences in GeneralPhysicsPublished by: -
2Articles: DFG German National LicensesStaff View
ISSN: 1476-4687Source: Nature Archives 1869 - 2009Topics: BiologyChemistry and PharmacologyMedicineNatural Sciences in GeneralPhysicsNotes: [Auszug] We have analysed data from the smallest field of view of the A2 experiment 0.18-2.5 keV detectors. This has dimensions of 1.55 FWHM in the scan direction (ecliptic latitude) and 3.1 FWHM in the perpendicular direction (ecliptic longitude). The total geometric area of the detector with this field ...Type of Medium: Electronic ResourceURL: -
3Articles: DFG German National LicensesCharles, P. A. ; Corbet, R. H. D. ; Mukai, K. ; Smale, A. P. ; Kahn, S. M. ; Kuhi, L. V. ; Brown, A.
Springer
Published 1985Staff ViewISSN: 1572-9672Source: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract A highly variable point X-ray source, first seen by the Einstein IPC, has been positioned with the EXOSAT CMA and identified with a bright (V = 8.5) K0 star. Although in the direction of the southern half of the Cygnus Loop, this star is almost certainly a foreground object and typical of other active cool stars that are related to RS CVn systems. An EXOSAT program to study T Tauri stars failed to detect T Tau itself. However, a strong X-ray source was observed 15′ from T Tau, which in its turn had not been seen by Einstein. This new source has been identified with a hitherto unstudied 13 mag star which is likely to be a dMe flare star. The young star cluster NGC 2264 was observed with the EXOSAT CMA in an attempt to identify the sources found during an Einstein IPC study of S Mon. Apart from S Mon itself, only UV-bright objects were seen, but several of these are considered likely counterparts of the Einstein sources.Type of Medium: Electronic ResourceURL: -
4Articles: DFG German National LicensesStaff View
ISSN: 1572-9672Source: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract Preliminary results of an EXOSAT observation of the transient X-ray source 4U1543-47 are presented. The source was observed in August 1983, during a high state, following a Tenma alert that the source was again active. Results from the GSPC and the LE 1000 l/mm grating are presented. The spectrum is complex, but in the 2–10 keV energy range can be well described by a Comptonised thermal distribution. Extrapolating the same model into the lower energy band of the grating requires an absorption column density equivalent to 2 × 1021 H cm2. A marked under-abundance of Oxygen and overabundance of Nitrogen, along with a strong, unidentified line feature at 9.8 Å, are necessary to model the grating data.Type of Medium: Electronic ResourceURL: -
5Articles: DFG German National LicensesMukai, K. ; Bonnet-Bidaut, J. M. ; Bowyer, S. ; Charles, P. A. ; Chiappetti, L. ; Clarke, J. T. ; Corbet, R. H. D. ; Henry, J. P. ; Hill, G. J. ; Kahn, S. M. ; Maraschi, L. ; Osborne, J. ; Treves, A. ; Klis, M. ; Paradijs, J. ; Vrtilek, S. D.
Springer
Published 1985Staff ViewISSN: 1572-9672Source: Springer Online Journal Archives 1860-2000Topics: PhysicsNotes: Abstract The AM Her type object E2003+225 was observed with EXOSAT, IUE and ground-based telescopes on 1983 Oct. 12. The brightness of the ultrasoft X-ray component allowed the Objective Grating Spectrometer (OGS) to be used, which gave a model-independent determination of the temperature of the blackbody spectrum. The star was observed again on 1984 July 24 by IUE with simultaneous optical spectrophotometry. The high resolution of this observation revealed complex line profiles, and a systematic velocity much smaller than previously reported. The composite energy distribution is presented.Type of Medium: Electronic ResourceURL: