Wed·May 18, 2022Wednesday·May 18, 2022

1. 01*

   Horizons: Nuclear Astrophysics in the 2020s and Beyond

   H. Schatz🇺🇸 · A. D. Becerril Reyes🇺🇸 · A. Best🇮🇹 · E. F. Brown🇺🇸 · K. Chatziioannou🇺🇸 · K. A. Chipps🇺🇸 · C. M. Deibel🇺🇸 · R. Ezzeddine🇺🇸 · D. K. Galloway🇦🇺 · C. J. Hansen🇩🇪 · F. Herwig🇨🇦 · A. P. Ji🇺🇸 and 153 other authors

   Nuclear Astrophysics is a field at the intersection of nuclear physics and astrophysics, which seeks to understand the nuclear engines of astronomical objects and the origin of the chemical elements. This white paper summarizes progress and status of the field, the new open questions that have emerged, and the tremendous scientific opportunities that have opened up with major advances in capabilities across an ever growing number of disciplines and subfields that need to be integrated. We take a holistic view of the field discussing the unique challenges and opportunities in nuclear astrophysics in regards to science, diversity, education, and the interdisciplinarity and breadth of the field. Clearly nuclear astrophysics is a dynamic field with a bright future that is entering a new era of discovery opportunities.

   nucl-exastro-ph.HEastro-ph.SRnucl-thJ.Phys.G(2022)·48 citations
2. 02*

   Proton capture on ${}^{30}$P in novae: On the existence of states at $6.40$ MeV and $6.65$ MeV in ${}^{31}$S

   M. Kamil🇿🇦 · S. Triambak🇿🇦 · G. C. Ball🇨🇦 · V. Bildstein · A. Diaz Varela🇨🇦 · T. Faestermann🇩🇪 · P. E. Garrett🇨🇦 · F. Ghazi Moradi🇨🇦 · R. Hertenberger🇩🇪 · N. Y. Kheswa🇿🇦 · N. J. Mukwevho🇿🇦 · B. M. Rebeiro🇫🇷 · H.-F.Wirth🇩🇪

   We use a high resolution ${}^{32}\mathrm{S}(d,t)$ measurement to investigate the claimed existence of a 6401(3) keV state in ${}^{31}$S that may affect the ${}^{30}\mathrm{P}(p,\gamma )$ nuclear reaction rate in oxygen-neon (ONe) novae. Our data are shown to exclude the null hypothesis - that the state does not exist - with high significance. Additionally, the data also suggest the existence of a hitherto unreported state at 6648(4) keV. This state corresponds to a ${}^{30}\mathrm{P}(p,\gamma )$ resonance at $517(4)$ keV, located below the higher edge of the Gamow window for peak nova temperatures of about 0.4 GK.

   nucl-exPRC(2022)·2 citations
3. 03*

   Semi-inclusive Diffractive Deep Inelastic Scattering at Small-$x$

   Yoshitaka Hatta🇺🇸 · Bo-Wen Xiao🇨🇳 · Feng Yuan🇺🇸

   Inspired by a recent study of Iancu, Mueller and Triantafyllopoulos [1] and earlier papers by Golec-Biernat and Wusthoff [2,3], we propose semi-inclusive diffractive deep inelastic scattering (SIDDIS) to investigate the gluon tomography in the nucleon and nuclei at small-$x$. The relevant diffractive quark and gluon parton distribution functions (DPDF) can be computed in terms of the color dipole S-matrices in the fundamental and adjoint representations, respectively. Novel correlations from the gluon tomography in the dipole S-matrix can be experimentally studied through the DPDFs in these processes at the future electron-ion collider (EIC).

   ↳ hep-phhep-exnucl-exnucl-thPRD(2022)·62 citations
4. 04*

   New Way to Resum the Lattice QCD Taylor Series Equation of State at Finite Chemical Potential

   Sabarnya Mitra🇮🇳 · Prasad Hegde🇮🇳 · Christian Schmidt🇩🇪

   Taylor expansion of the thermodynamic potential in powers of the (baryo)chemical potential ${\mu }_B$ is a well-known method to bypass the Sign Problem of Lattice QCD. Due to the difficulty in calculating the higher order Taylor coefficients, various alternative expansion schemes as well as resummation techniques have been suggested to extend the Taylor series to larger values of ${\mu }_B$. Recently, a way to resum the contribution of the first $N$ charge density correlation functions $D_1,\dots ,D_N$ to the Taylor series to all orders in ${\mu }_B$ was proposed in Phys. Rev. Lett. 128, 2, 022001 (2022). The resummation takes the form of an exponential factor. Since the correlation functions are calculated stochastically, the exponential factor contains a bias which can be significant for large $N$ and ${\mu }_B$. In this paper, we present a new method to calculate the QCD equation of state based on the well-known cumulant expansion from statistics. By truncating the expansion at a maximum order $M$, we end up with only finite products of the correlation functions which can be evaluated in an unbiased manner. Although our formalism is also applicable for ${\mu }_B\ne 0$, here we present it for the simpler case of a finite isospin chemical potential ${\mu }_I$ for which there is no Sign Problem. We present and compare results for the pressure and the isospin density obtained using Taylor expansion, exponential resummation and cumulant expansion, and provide evidence that the absence of bias in the latter actually improves the convergence.

   ↳ hep-lathep-phnucl-exnucl-thPRD(2022)·26 citations

* Reconstructed cohort: no mailing for this day survives in the archive. Papers are grouped by their submission times and arXiv's announcement cut-off, assuming announcement without delay; positions follow identifier order. Validated at ~91% exact-day agreement against the archived era.