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X-Ray Emission and Corona of the Young Intermediate-Mass Binary θ1 Ori E

  • Authors: David P. Huenemoerder, Norbert S. Schulz, Paola Testa, Anthony Kesich, and Claude R. Canizares

HUENEMOERDER et al. 2009 The Astrophysical Journal 707 942.

  • Provider: AAS Journals

Caption: Figure 6.

Stars listed in Table 7 are shown on a temperature–luminosity diagram. Pre-main-sequence stars are shown with open symbols and post-main-sequence stars are shown as solid symbols. The shapes encode L x / L bol as a "star" for ⩾10 −3, circle for ⩾10 −4 to <10 −3, and a square for <10 −5 (see Table 7 for values). The PMS evolutionary tracks (thick gray lines) and ZAMS are from Siess et al. (2000). The post-main-sequence tracks (thin gray lines) are from Schaller et al. (1992). The tracks are shown for 2  M , 3  M ,  and 4  M . The post-main-sequence tracks were scaled slightly (0%–3% in temperature, 8%–12% in luminosity) to better coincide with the PMS tracks.)

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