Solar Physics

, Volume 187, Issue 2, pp 229–260 | Cite as

The transition region and coronal explorer

  • B.N. Handy
  • L.W. Acton
  • C.C. Kankelborg
  • C.J. Wolfson
  • D.J. Akin
  • M.E. Bruner
  • R. Caravalho
  • R.C. Catura
  • R. Chevalier
  • D.W. Duncan
  • C.G. Edwards
  • C.N. Feinstein
  • S.L. Freeland
  • F.M. Friedlaender
  • C.H. Hoffmann
  • N.E. Hurlburt
  • B.K. Jurcevich
  • N.L. Katz
  • G.A. Kelly
  • J.R. Lemen
  • M. Levay
  • R.W. Lindgren
  • D.P. Mathur
  • S.B. Meyer
  • S.J. Morrison
  • M.D. Morrison
  • R.W. Nightingale
  • T.P. Pope
  • R.A. Rehse
  • C.J. Schrijver
  • R.A. Shine
  • L. Shing
  • K.T. Strong
  • T.D. Tarbell
  • A.M. Title
  • D.D. Torgerson
  • L. Golub
  • J.A. Bookbinder
  • D. Caldwell
  • P.N. Cheimets
  • W.N. Davis
  • E.E. Deluca
  • R.A. McMullen
  • H.P. Warren
  • D. Amato
  • R. Fisher
  • H. Maldonado
  • C. Parkinson
Article

Abstract

The Transition Region and Coronal Explorer (TRACE) satellite, launched 2 April 1998, is a NASA Small Explorer (SMEX) that images the solar photosphere, transition region and corona with unprecedented spatial resolution and temporal continuity. To provide continuous coverage of solar phenomena, TRACE is located in a sun-synchronous polar orbit. The ∼700 Mbytes of data which are collected daily are made available for unrestricted use within a few days of observation. The instrument features a 30-cm Cassegrain telescope with a field of view of 8.5×.5 arc min and a spatial resolution of 1 arc sec (0.5 arc sec pixels). TRACE contains multilayer optics and a lumogen-coated CCD detector to record three EUV wavelengths and several UV wavelengths. It observes plasmas at selected temperatures from 6000 K to 10 MK with a typical temporal resolution of less than 1 min.

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Copyright information

© Kluwer Academic Publishers 1999

Authors and Affiliations

  • B.N. Handy
    • 1
  • L.W. Acton
    • 1
  • C.C. Kankelborg
    • 1
  • C.J. Wolfson
    • 2
  • D.J. Akin
    • 2
  • M.E. Bruner
    • 2
  • R. Caravalho
    • 2
  • R.C. Catura
    • 2
  • R. Chevalier
    • 2
  • D.W. Duncan
    • 2
  • C.G. Edwards
    • 2
  • C.N. Feinstein
    • 2
  • S.L. Freeland
    • 2
  • F.M. Friedlaender
    • 2
  • C.H. Hoffmann
    • 2
  • N.E. Hurlburt
    • 2
  • B.K. Jurcevich
    • 2
  • N.L. Katz
    • 2
  • G.A. Kelly
    • 2
  • J.R. Lemen
    • 2
  • M. Levay
    • 2
  • R.W. Lindgren
    • 2
  • D.P. Mathur
    • 2
  • S.B. Meyer
    • 2
  • S.J. Morrison
    • 2
  • M.D. Morrison
    • 2
  • R.W. Nightingale
    • 2
  • T.P. Pope
    • 2
  • R.A. Rehse
    • 2
  • C.J. Schrijver
    • 2
  • R.A. Shine
    • 2
  • L. Shing
    • 2
  • K.T. Strong
    • 2
  • T.D. Tarbell
    • 2
  • A.M. Title
    • 2
  • D.D. Torgerson
    • 2
  • L. Golub
    • 3
  • J.A. Bookbinder
    • 3
  • D. Caldwell
    • 3
  • P.N. Cheimets
    • 3
  • W.N. Davis
    • 3
  • E.E. Deluca
    • 3
  • R.A. McMullen
    • 3
  • H.P. Warren
    • 3
  • D. Amato
    • 4
  • R. Fisher
    • 4
  • H. Maldonado
    • 4
  • C. Parkinson
    • 4
  1. 1.Department of PhysicsMontana State University–BozemanBozemanU.S.A
  2. 2.Lockheed Martin Palo Alto Advanced Technology Center, O/L9-41Palo AltoU.S.A
  3. 3.Smithsonian Astrophysical ObservatoryCambridgeU.S.A
  4. 4.NASA/Goddard Space Flight CenterGreenbeltU.S.A

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