tokens: ( 1996 ) and find thatThis implies that the disk is not very thin. From the vales in Equations ( 7 )–( 9 ) we can calculate the typical neutrino cooling timescale in the disk. Taking the neutrino cooling rate as (Brown Weingartner 1994 ) , we calculate the neutrino cooling timescaleWe calculate the radial velocity in the disk from mass accretion rate and find it to be . The inflow time of the gas in the disk from is . Namely, neutrino cooling in the disk is important. From the above results we can safely conclude that our derivations are self-consistent and that neutrino cooling plays a major role in the accretion disk of our scenario. Neutrino cooling lowers the temperature of the accreted gas, reducing the pressure and ensuring a mildly electron degenerate state, as in the scenario of Siegel et al. ( 2019 ). From Beloborodov ( 2003 ) the electrons become degenerate below the characteristic degeneracy temperature ofThis is somewhat higher than the typical temperature we find in Equation ( 9 ), implying that we have a mildly degenerate electron gas as Siegel et al. ( 2019 ) find in their scenario. Moreover, according to Figure 1 of Beloborodov ( 2003 ), the baryonic matter in the accretion disk of our scenario is in nuclear statistical equilibrium and is dominated by free nucleons with an electron-to-baryon ratio of Y e 0.3, i.e., a large fraction of neutron to protons. Overall, we conclude that the accretion disk conditions in the CEJSN r -process scenario resemble the conditions from the studies of Kohri et al. ( 2005 ) and Siegel et al. ( 2019 ). We expect then the outflow properties to be quite similar. 5.3. Nucleosynthesis in Jets As we mention above, at the stage of high mass accretion rate the core mass inner to the orbit of the NS is ≈1 M ⊙ . A large fraction of this mass is expected to be accreted at this high rate. As described in Section 2 , Papish et al. ( 2015 ) estimated that the jets in the CEJSN r -process scenario are expected to synthesize a mass of ≈0.001–0.01 M ⊙ of heavy r -process elements per event. This is based on the assumption that a fraction of ≈10% of the accreted mass is launched in the jets and ≈10% of the mass in the jets is transferred to heavy r -process elements. If we had used the recent results of Siegel et al. ( 2019 ), the mass of the r -process elements would have been even higher. Siegel et al. ( 2019 ) find the ejected mass to be ≈30% of the accreted mass. Under this assumption, we can take a more optimistic yield than what Papish et al. ( 2015 ) used, namely, we can take the yield per CEJSN r -process event to be ≈0.01–0.03 M ⊙ of heavy r -process elements. As we mentioned in Section 2 , Chevalier ( 2012 ) estimated the rate of events in which an NS enters the envelope of a giant star to be ≈1% of the total rate of CCSNe. Papish et al. ( 2015 ) found that if this is also the rate of CEJSN r -process events, then combining it with the yield of r -process elements that they derived, we obtain the
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