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.
- Experimental study of the Si-30(He-3, d) P-31 reaction and thermonuclear reaction rate of Si-30(p, gamma)( 3)1P , PHYSICAL REVIEW C (2022)
- New energy for the 133-keV resonance in the Na-23(p, gamma) Mg-24 reaction and its impact on nucleosynthesis in globular clusters , PHYSICAL REVIEW C (2021)
- Bayesian analysis of the Zn-70(d, He-3) Cu-69 transfer reaction , PHYSICAL REVIEW C (2020)
- Correlated energy uncertainties in reaction rate calculations , ASTRONOMY & ASTROPHYSICS (2020)
- Evaluation of the N-13(alpha, p)O-16 thermonuclear reaction rate and its impact on the isotopic composition of supernova grains , PHYSICAL REVIEW C (2020)
- Shell-model studies of the astrophysical rp-process reactions S-34(p, gamma) Cl-35 and Cl-34g(,m)(p, gamma) Ar-35 , PHYSICAL REVIEW C (2020)
- Shell-model studies of the astrophysical rp-process reactions S-34(p,gamma)Cl-35 and Cl-34g,Cl-m(p,gamma)Ar-35 , 27TH INTERNATIONAL NUCLEAR PHYSICS CONFERENCE (INPC2019) (2020)
- Study of the Mg-25(d,p)Mg-26 reaction to constrain the Al-25(p,gamma)Si-26 resonant reaction rates in nova burning conditions , EUROPEAN PHYSICAL JOURNAL A (2020)
- Thermonuclear reaction rate of Si-30(p , gamma) P-31 , PHYSICAL REVIEW C (2020)
- Experimental study of Cl35 excited states via S32(α,p) , Physical Review C (2019)