The main fusion reaction in the sun is the proton-proton chain reaction, which takes six protons and produces two protons, one alpha particle, two anti-electrons, and two electron neutrinos.
The deuterium nucleus is only barely bound and can be destroyed — dissociated into a proton and neutron — by absorbing a gamma ray with energy more than 2 MeV. This means that all of the sun's "primordial" deuterium, formed in the first minutes after the Big Bang, was destroyed before the sun got hot enough to begin fusing on its own. Essentially all of the deuterium in the sun exists as an intermediate step in the proton-proton fusion cycle.
Tritium, furthermore, is naturally unstable, with a half-life of only 12 years. This means that any tritium in the sun (or anywhere else) has been mostly produced in the past few dozen years. On Earth tritium is produced by cosmic rays interacting with stable matter. In the sun most of the tritium would come from neutron capture on deuterium (where I suppose the neutrons would have come from dissociated deuterium) or nucleon-exchange or proton-knockout reactions on helium-3 and helium-4.
A relatively authoritative solar model I grabbed some time ago from this paper (or more properly, from here) lists the helium-3 fraction, but not the deuterium fraction or tritium fraction. If we assume they are comparable (or at least related) then you can see that it still depends on where you are in the sun:
For what it's worth, more than 99% of the sun's energy is produced deeper in than that peak at 0.27 R_sun.