Richard Longland
Bio
After graduating from the University of Surrey, England, with an MPhys degree in Physics with Satellite Technology, Richard Longland moved to the U.S. to pursue a PhD in Nuclear Astrophysics at the University of North Carolina at Chapel Hill in 2004. His thesis work (under the direction of Prof. Christian Iliadis) concentrated on characterising neutron producing reactions in massive stars and Asymptotic Giant Branch (AGB) stars. He also developed Monte Carlo methods for calculating the uncertainties on nuclear reaction rates in stars, which continues to be a key factor in his research today.
In 2010, Richard moved to Barcelona, Spain, to work with Jordi José at the Universitat Politècnica de Catalunya and broaden his experience in nuclear astrophysics. While there, he developed parallel processing nucleosynthesis models to investigate Monte Carlo sensitivity studies in AGB stars, novae, X-ray bursts, and low-mass white dwarf mergers. Using these methods, he was able to perform detailed nucleosynthesis studies to investigate the origin of R Corona Borealis stars.
Area(s) of Expertise
Richard's over-arching research goal is to understand the origin of the elements and how stars burn their fuel. Almost all of the elements heavier than helium in the solar system were made in stars. The rate of this synthesis by nuclear reactions also governs energy production, and thus the physical structure of stellar environments. To better understand these reactions and how stars burn their fuel, his research group focuses on precisely determining their cross sections in the laboratory. A combination of direct and indirect techniques are used to characterise the nuclear properties of the reactions and their products at the Triangle Universities Nuclear Laboratory (TUNL). In particular, his group uses the only functioning high resolution particle spectrometer dedicated to nuclear astrophysics experiments in North America. This spectrometer allows them to perform charge-exchange and particle transfer measurements, thus providing astrophysicists with critical information where more traditional direct cross section measurements are not feasible. By collaborating with stellar modellers and astronomers, these measurements are used to help improve our understanding of stars and how the elements were made.
Publications
- Decoding γ -ray signatures from core-collapse supernovae: First experimental constraints on the Al 28 ( p , α ) Mg 25 reaction rate , Physical Review C (2026)
- The 2025 Evaluation of Experimental Thermonuclear Reaction Rates (ETR25) , The Astrophysical Journal Supplement Series (2026)
- Bayesian analysis of the Sr 86 ( α , α ) reaction to constrain the Sr 86 ( α , n ) cross section at astrophysical energies , Physical Review C (2025)
- Data for the 2025 Evaluation of Experimental Reaction Rates (ETR25) , Zenodo (CERN European Organization for Nuclear Research) (2025)
- Data for the 2025 Evaluation of Experimental Reaction Rates (ETR25) , Zenodo (CERN European Organization for Nuclear Research) (2025)
- Erratum: “Low-metallicity Nova Explosions: A Site for Weak rp-process Nucleosynthesis” (2025, ApJ, 987, 88) , The Astrophysical Journal (2025)
- Indirect measurement of the Na 23 ( p , γ ) Mg 24 direct capture reaction rate via ( He 3 , d ) spectroscopy , Physical Review C (2025)
- Inverse kinematics study of the energy levels of Ne 21 populated with the Ne 20 + d reaction , Physical Review C (2025)
- Investigation of P 31 levels near the proton threshold with nuclear resonance fluorescence and the impact on the Si 30 ( p , γ ) P 31 thermonuclear rate , Physical Review C (2025)
- Low-metallicity Nova Explosions: A Site for Weak rp-process Nucleosynthesis , The Astrophysical Journal (2025)