Discovery of X-ray and Extreme Ultraviolet Emission from Comet C/Hyakutake 1996 B2-Reference-Cited by-同舟云学术

Discovery of X-ray and Extreme Ultraviolet Emission from Comet C/Hyakutake 1996 B2

Published:1996-10-11 Issue:5285 Volume:274 Page:205-209
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Lisse C. M.¹,Dennerl K.²,Englhauser J.²,Harden M.³,Marshall F. E.⁴,Mumma M. J.⁴,Petre R.⁴,Pye J. P.⁵,Ricketts M. J.³,Schmitt J.²,Trümper J.²,West R. G.⁵

Affiliation:

1. C. M. Lisse is in the Astronomy Department, University of Maryland, College Park, MD 20742, and NASA Goddard Spaceflight Center, Greenbelt, MD 20771, USA.

2. K. Dennerl, J. Englhauser, J. Schmitt, and J. Trümper are at the Max-Planck-Institut für Extraterrestriche Physik, Postfach 1603, 85740 Garching, Germany.

3. M. Harden and M. J. Ricketts are in the Space and Astrophysics Division, Rutherford Appleton Laboratory, Chilton, Didcot, Oxon, OX11 0QX, UK.

4. F. E. Marshall, M. J. Mumma, and R. Petre are at the NASA Goddard Spaceflight Center, Greenbelt, MD 20771, USA.

5. J. P. Pye and R. G. West are in the Department of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference30 articles.

1. Trümper J., Adv. Space. Res. 2, 241 (1983).

2. Schmitt J. H. M. M., ibid. 11 125 1991. The ROSAT HRI is a microchannel plate detector coupled to a grazing incidence telescope with an effective area of ∼20 cm2 at 0.1 to 2.0 keV, a circular FOV 38′ in diameter, and an angular resolution of 6 inches HEW (half-energy width) (1, 2). Coarse pulse height discrimination is used to distinguish UV sources from x-ray emitting objects. The ROSAT WFC has three concentric gold-plated mirrors coupled to a curved microchannel plate at the focal plane, providing a circular FOV of 5° in diameter with an angular resolution of 2′ HEW [M. R. Sims et al. Opt. Eng. 29, 649 (1990) and J. P. Pye et al. Mon. Not. R. Astron. Soc. 274, 1165. (1995)]. All of our WFC observations were obtained with the S1A filter, with a nominal bandpass (at 10% of peak effective area) of 90 to 206 eV and an on-axis effective area of ∼1 cm2. Lack of contamination from UV red leaks (wavelength >1000 Å) has been established by the non-detection of the bright A0 star Vega at a 90% confidence upper limit of 5 × 10−4 counts s−1. The optical axes of the HRI and WFC are co-aligned to within 10 to 15′, providing simultaneous observations in the EUV and x-ray. The backgrounds in both instruments are dominated by particles, and must be removed by modeling [S. L. Snowden, personal communication and R. G. West, Thesis, University of Leicester (1993)].

3. The XTE PCA consists of five non-imaging multiwire proportional counters and has an effective area of about 6500 cm 2 [W. Zhang et al. in Proc. SPIE 2006 324 (1993)]. The PCA detects x-rays in the 2- to 60-keV band with an FOV diameter of about 2°. Background confusion noise dominates the observations in the PCA.

4. Ibadov S., Icarus 86, 283 (1990).

5. Reme H., et al., Astron. Astrophys. 187, 33 (1987).

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