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hot-CNO and breakout

hot-CNO and breakout#

import pynucastro as pyna

This collection of rates has the main CNO rates plus a breakout rate into the hot CNO cycle(s)

rl = pyna.ReacLibLibrary()

We’ll get all the rates linking the core nuclei in CNO and the various hot-CNO cycles, but we’ll explicitly remove \(3\)-\(\alpha\), since it is not strong at the temperatures where CNO operates.

linking_nuclei = ["p", "he4",
                  "c12", "c13",
                  "n13", "n14", "n15",
                  "o14", "o15",]
lib = rl.linking_nuclei(linking_nuclei, with_reverse=False)
r3a = lib.get_rate_by_name("he4(aa,g)c12")
lib.remove_rate(r3a)

rc = pyna.RateCollection(libraries=lib)

To evaluate the rates, we need a composition. This is defined using a list of Nucleus objects.

comp = pyna.Composition(rc.get_nuclei())
comp.set_solar_like()

Transition from CNO to hot-CNO#

Let’s look at the CNO cycle at a temperature and density just a bit hotter than the Sun’s core

T = 2.e7
rho = 200

fig = rc.plot(rho=rho, T=T, comp=comp, ydot_cutoff_value=1.e-20)
../_images/41f436afb634bac1dae8374ef0d294244758478ad64d07c26af319ff19b83957.png

Starting at \({}^{12}\mathrm{C}\), we see the following sequence dominate:

  • We capture a proton to make \({}^{13}\mathrm{N}\)

  • \({}^{13}\mathrm{N}\) almost immediately beta decays to \({}^{13}\mathrm{C}\), since the beta-decay rate is so much faster than a proton capture on \({}^{13}\mathrm{N}\).

  • We continue with proton captures, making \({}^{14}\mathrm{N}\) and then \({}^{15}\mathrm{O}\)

  • \({}^{15}\mathrm{O}\) then beta-decays to get \({}^{15}\mathrm{N}\)

  • Finally, one last proton capture, doing \({}^{15}\mathrm{N}(p,\alpha){}^{12}\mathrm{C}\), getting us back to where we started.

This is the basic CNO cycle

Now let’s make it a bit hotter

T = 3.e8
fig = rc.plot(rho=rho, T=T, comp=comp, ydot_cutoff_value=1.e-20)
../_images/42e27e188b13c70829275798ff9f66efad65592e64986394a41cd6c8d9698a6c.png

Now we see that the proton capture on \({}^{13}\mathrm{N}\) is faster than the beta-decay, and we make \({}^{14}\mathrm{O}\). Then the cycle continues as before.

As we increase the temperature and density further, we see that the beta decays become the rate-limiting steps.

T = 5.e8
rho = 1.e4
fig = rc.plot(rho=rho, T=T, comp=comp, ydot_cutoff_value=1.e-20)
../_images/f911285ee8f5d47c4fbf24ba18b234254499d06d2b0163ee90f74265f530529a.png

Since the beta-decays are temperature independent (you just have to wait for the nucleus to decay), the overall hot-CNO rate becomes insensitive to temperature.

When does hot-CNO set in?#

We can look at the temperature where we cross from CNO to hot-CNO by looking at the rates involving \({}^{13}\mathrm{N}\)

r1 = rl.get_rate_by_name("n13(p,g)o14")
r2 = rl.get_rate_by_name("n13(,)c13")

import numpy as np
import matplotlib.pyplot as plt

T = np.logspace(7.5, 8.5, 100)

rate_p_capture = [r1.eval(temp) for temp in T]
rate_beta_decay = [r2.eval(temp) for temp in T]

fig, ax = plt.subplots()
ax.plot(T, rate_p_capture, label=r"${}^{13}\mathrm{N}(p,\gamma){}^{14}\mathrm{O}$")
ax.plot(T, rate_beta_decay, label=r"${}^{13}\mathrm{N} \rightarrow {}^{13}\mathrm{C}$")
ax.legend()
ax.set_xscale("log")
ax.set_yscale("log")
../_images/fb195e2833e6fa40da109d2820850885e6009f4acaa065a87a5c923b3b0829ff.png

We see that above \(T \sim 2\times 10^8~\mathrm{K}\), the proton-capture proceeds faster than the beta-decay, and we transition to hot-CNO.

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