Addendum: ``Heating in the Accreted Neutron Star Ocean: Implications for Superburst Ignition'' (ApJ, 662, 1188 [2007])

Details Addendum: ``Heating in the Accreted Neutron Star Ocean: Implications for Superburst Ignition'' (ApJ, 662, 1188 [2007]) Addendum: ``Heating in the Accreted Neutron Star Ocean: Implications for Superburst Ignition'' (ApJ, 662, 1188 [2007])

Jan 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...672.1292g&link_type=abstract

The Astrophysical Journal, Volume 672, Issue 2, pp. 1292-1292.

Astronomy and Astrophysics

Astronomy

Errata, Addenda

Scientific paper

For convenience in constructing numerical models, we here append Table A1, giving the data used to generate Figure 7. We give the value of the heat deposition, Q, for a given mass chain A as a function of the electron chemical potential μe for μe<20 MeV (ρYe~6×1010 g cm-3, where Ye is the electron abundance). Note that μe does not include the electron rest mass. We calculate Q according to the approximate model described in § 3.3. Table A1 lists for each mass chain A (col. [1]) the charge number Zi of the nucleus entering each transition (col. [2]), the charge number Zf of the nucleus after all allowed captures have occurred (col. [3]), the electron chemical potential μe of the transition (col. [4]), and the net heat deposited per nucleon Q by these captures into the neutron star crust (col. [5]). Note that in many cases the first capture onto nucleus AZi is immediately followed by a second capture, which is why there are numerous entries with Zi-Zf=2. For a multicomponent plasma, one should multiply the heat deposition Q of a particular transition by the mass fraction for that A.

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