Scientific and Technical Aerospace Reports Volume 38 July 28, 2000

Title (LMSAL) lead the optical imaging team. The optical telescope is a 50-cm aperture, diffraction limited, Gregorian. The focal
plane package will record high resolution images, Dopplergrams, and vector magnetic fields on spatial scales dominated by elemental
photospheric flux tubes, and over a field of view large enough to contain small active regions. Drs. Tetsuya Watanabe, Len
Culhane (MSSL) and George Doschek (NRL) led the EUV imaging and spectroscopy team. The EUV telescope has a 15-cm primary
mirror feeding a toroidal grating. The optics have multiplayer coatings which select two wavebands between 180-204 A
and 250-290 A. Drs. Kiyoto Shibasaki (NAOJ) and Leon Golub (SAO) lead the X-ray imaging team. The x-ray telescope will
provide full disk, soft x-ray images with twice the spatial resolution of the Yohkoh SXT and enhanced sensitivity to longer (>40
A) wavelengths. The launch of Solar-B, into a sun-synchronous orbit, is scheduled for August 2004. Solar-B is the second mission
in the Sun-Earth Connection, Solar-Terrestrial Probe Program which is managed by the Goddard Space Flight Center. The Science
Directorate of the Marshall Space Flight Center manages the Solar-B Project for the ST Probe Project Office. This paper discusses
the objectives, specifications, and design of the scientific instruments as presented at the Preliminary Design Review held at
MSFC in May 2000.
Author
Space Missions; Solar Atmosphere; Photosphere; X Ray Imagery; Solar Terrestrial Interactions
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20000063513 Smithsonian Astrophysical Observatory, Cambridge, MA USA
A Comparison of the Extra Nuclear X-ray and Radio Features in M87
Harris, D. E., Smithsonian Astrophysical Observatory, USA; Owen, F., National Radio Astronomy Observatory, USA; Biretta,
J. A., Space Telescope Science Inst., USA; Junor, W., New Mexico Univ., USA; Feb. 24, 2000; 4p; In English
Contract(s)/Grant(s): NAS5-99002; NSF AST-98-0307
Report No.(s): astro-ph/0002464; No Copyright; Avail: CASI; A01, Hardcopy; A01, Microfiche
ROSAT High Resolution Imager (HRI) data from eight observations have been co-added to obtain an effective exposure of
230 ksec. We have identified a number of features and regions with excess X-ray brightness over that from a circularly symmetric
model of the well known hot gas component. A prominent ’spur’ extends 4feet from the vicinity of knot A towards the south-west.
The brightness to the south and east of this spur is significantly higher than that to the north and west. Excess brightness is also
found to the East of the nucleus, with a local maximum centered on the eastern radio lobe 3 feet from the core. There are two well
known relationships between radio and X-ray emission for radio galaxies in clusters: coincidence of emissions because the X-rays
come from inverse Compton or synchrotron processes; and anti-coincidence caused by exclusion of hot gas from radio entities.
We present a radio/X-ray comparison to determine if either of these relationships can be isolated in M87. The greatest obstacle
we face is the unknown projection which affects both bands.
Author
X Rays; Brightness; Exposure; Radio Emission; Image Resolution
20000064086 Smithsonian Astrophysical Observatory, Cambridge, MA USA
X-Ray Variability in M87 Final Report, 1 Jul. 1997 - 30 Oct. 1999
Harris, Daniel E., Smithsonian Astrophysical Observatory, USA; Biretta, J. A., Space Telescope Science Inst., USA; Junor, W.,
New Mexico Univ., USA; June 2000; 24p; In English
Contract(s)/Grant(s): NAG5-4830
Report No.(s): Preprint-Series-4458; No Copyright; Avail: CASI; A03, Hardcopy; A01, Microfiche
We present the evidence for X-ray variability from the core and from knot A in the M87 jet based on data from two observations
with the Einstein Observatory High Resolution Imager (HRI) and three observations with the ROSAT HRI. The core intensity
showed a 16% increase in 17 months (’79-’80); a 12% increase in the 3 years ’92 to ’95; and a 17% drop in the last half of
1995. The intensity of knot A appears to have decreased by 16% between 92Jun and 95Dec. Although the core variability is consistent
with general expectations for AGB nuclei, the changes in knot A provide constraints on the x-ray emission process and geometry.
Thus we predict that the x-ray morphology of knot A will differ significantly from the radio and optical structure.
Author
X Rays; Variability; Active Galactic Nuclei; Elliptical Galaxies; Luminous Intensity