Erratum: ``Grain Properties of Comet C/1995 O1 (Hale-Bopp)'' (ApJ, 580, 579 [2002])

Details Erratum: ``Grain Properties of Comet C/1995 O1 (Hale-Bopp)'' (ApJ, 580, 579 [2002]) Erratum: ``Grain Properties of Comet C/1995 O1 (Hale-Bopp)'' (ApJ, 580, 579 [2002])

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...615.1081h&link_type=abstract

The Astrophysical Journal, Volume 615, Issue 2, pp. 1081-1081.

Astronomy and Astrophysics

Astronomy

16

Errata, Addenda

Scientific paper

In our original paper, the parameters for the best-fit model SEDs in Table 3 and the derived mass ratio of the total of submicron-sized grains listed in Table 4 were incorrectly quoted. For comet C/1995 O1 (Hale-Bopp), for the four epochs UT 1996 September/October (rh=2.8 AU), 1997 February (rh=1.21 AU), 1997 April (rh=0.93 AU), and 1997 June (rh=1.7 AU), the SED model fits shown respectively in Figures 6-9 utilize Np(crystalline olivine) larger than that quoted in Table 3 of the original paper. We have corrected this error in the revised Table 3 given here. This error was propagated into Table 4, which also used incorrect uniform bulk densities for all minerals in deriving the ratios of submicron grain abundances. A corrected Table 4 is given below, using the corrected bulk density of ρC=2.5 g cm-3 for carbon grains and of ρSi=3.3 g cm-3 for silicate grains, and taking into account that the submicron amorphous carbon and amorphous silicate grains are porous (model parameter D<3). For the total population of submicron grains, the derived silicate-to-amorphous carbon ratio is in the range of 8.1-13.3, significantly higher than the range of 3.8-4.5 quoted in our original paper. Furthermore, for comet Hale-Bopp the silicate crystalline-to-amorphous ratio spans the range 1.5-3.7, 3 to 4 times greater than the range of crystalline silicate/amorphous silicate = 0.5-0.9 originally quoted by us.

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