2021FRIB/NSCL Graduate Brochure

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Alex Brown Professor of Physics Theoretical Nuclear Physics BA, Physics, Ohio State University, 1970 MS, Physics, SUNY Stony Brook, 1972 PhD, Physics, SUNY Stony Brook, 1974 Joined NSCL in January 1982 brown@nscl.msu.edu Selected Publications Microscopic calculations of nuclear level densities with the Lanczos method, W. E. Ormand, and B. A. Brown, Phys. Rev. C 102, 014315 (2020), New Isospin-Breaking USD Hamiltonians for the sd-shell, A. Magilligan and B. A. Brown, Phys. Rev. C 101, 064303 (2020), Implications of the 36 Ca- 36 S and 38Ca- 38Ar difference in mirror charge radii on the neutron matter equation of state, B. A. Brown, et al., Phys. Rev. Research 2, 0223035(R) (2020). Constraints on Skyrme equations of state from doubly magic nuclei, ab initio calculations of low-density neutron matter, and neutron stars. Y. Tsang, B. A. Brown, F. J. Fattoyev, W. G. Lynch, and M. B. Tsang, Phys. Rev. C 100, 062801(R) (2019). My research in theoretical nuclear physics is motivated by broad questions in science: What are the fundamental particles of matter? What are the fundamental forces and their symmetries that govern their interactions? How were the elements formed during the evolution of the Universe? How do the simplicities observed in many-body systems emerge from their underlying microscopic properties? Specific topics of interest include: the structure of light nuclei and nuclei near the driplines, di-proton decay, proton and neutron densities, double β decay, isospin non-conservation, level densities, quantum chaos, nuclear equations of state for neutron stars, and the rapid-proton capture process in astrophysics. The diverse activities within our nuclear theory group, coupled with the forefront experimental work in nuclear structure, nuclear reactions and nuclear astrophysics at NSCL provide the perfect environment for the development of new theoretical ideas. I also have collaborations with theoretical and experimental groups in many countries including Germany, France, England, Italy, Norway, Japan, and South Africa. I pursue the development of new analytical and computational tools for the description of nuclear structure, especially for nuclei far from stability. The basic theoretical tools include the configuration-interaction and energydensity functional methods. I work with collaborators to developed software for desktop computing as well for highperformance computing. KEYWORDS Configuration Interaction Theory | Energy Density Functional Theory | Applications to Nuclear Structure and Astrophysics | Applications to Fundamental Interactions 26
Edward Brown Professor of Physics Theoretical Nuclear Astrophysics Selected Publications Rapid Neutrino Cooling in the Neutron Star MXB 1659-29, E. F. Brown, A. Cumming, F. J. Fattoyev, C. J. Horowitz, D. Page, and S. Reddy, Physical Review Letters, 120, 182701 (2018). Lower limit on the heat capacity of the neutron star core, A. Cumming, E. F. Brown, F. J. Fattoyev, C. J. Horowitz, D. Page, and S. Reddy, Physical Review C, 95, 025806 (2017) A Strong Shallow Heat Source In the Accreting Neutron Star MAXI J0556-332, A. Deibel, A. Cumming, E.F. Brown, and D. Page, Astrophys. Jour. Lett., 809, L31 (2015). Strong neutrino cooling by cycles of electron capture and β-decay in neutron star crusts, H. Schatz et al., Nature, 505, 62 (2014) The Equation of State from Observed Masses and Radii of Neutron Stars, A. W. Steiner, J. M. Lattimer, and E. F. Brown, Astrophys. J. 722, 33 (2010) BS, Physics, The Ohio State University, 1993 MS, Physics, University of California, Berkeley, 1996 PhD, Physics, University of California, Berkeley, 1999 Joined NSCL in February 2004 browne@nscl.msu.edu Formed in the violent death of a massive star, neutron stars are the most dense objects in nature. Their cores may reach several times the density of an atomic nucleus. As a result, neutron stars are a natural laboratory to study dense matter in bulk. We have observed neutron stars with telescopes, captured neutrinos from the birth of a neutron star, and detected gravitational waves from a neutron star merger. These observations complement laboratory studies of matter at super-nuclear density. My work connects observations of neutron stars with theoretical and laboratory studies of dense matter. Many neutron stars reside in binaries accrete gas from a binary, solar-like companion. The weight of this accumulated matter compresses the outer layer, or crust, of the neutron star and induces nuclear reactions. These reactions power phenomena over timescales from seconds to years. By modeling these phenomena and comparing with observatons, we can infer properties of dense matter in the neutron star’s crust and core. Recently, we have set a lower bound on the heat capacity of one neutron star and to inferred the efficiency of neutrino emission from the core of another. We have also calculated, using realistic nuclear physics input, reactions in the crust of accreting neutron stars. These calculations quantified the heating of the neutron star from these reactions, and the results have been used in simulations of the “freezing” of ions into a lattice in the neutron star crust. A surprise from these simulations is that the “ashes” of these bursts chemically separate as they are compressed to high densities. This may explain the inferred high thermal conductivity of the neutron star’s crust. Cutaway of the neutron star in MAXI J0556-332. During accretion, the outermost kilometer of the neutron star—its crust—is heated by compression-induced reactions (inset plot, which shows the temperature within the crust over a span of 500 days). When accretion halts (at time 0 in the plot), the crust cools. By monitoring the surface temperature during cooling, Deibel et al. determined that a strong heat source must be located at a relatively shallow depth of approximately 200 meters. KEYWORDS Equation of State | Neutron Stars Dense Matter | Stellar Modeling 27
Page 3 and 4: TABLE OF CONTENTS 1 TABLE OF CONTEN
Page 5 and 6: As a campus-based national user fac
Page 7 and 8: NUCLEAR SCIENCE AT MSU Nuclear scie
Page 9 and 10: On March 19, 2020, FRIB accelerated
Page 11 and 12: MSU CRYOGENIC INITIATIVE The demand
Page 13 and 14: FRIB THEORY ALLIANCE The FRIB Theor
Page 15 and 16: GRADUATE STUDENT LIFE When you are
Page 17 and 18: CAREERS Your success as a graduate
Page 19 and 20: ANIA KWIATKOWSKI PhD IN PHYSICS, 20
Page 21 and 22: THE LANSING AREA Capital city Lansi
Page 23 and 24: Recreation Many recreational activi
Page 25 and 26: Daniel Bazin Research Senior Physic
Page 27: Georg Bollen University Distinguish
Page 31 and 32: Kaitlin Cook Assistant Professor of
Page 33 and 34: Pawel Danielewicz Professor of Phys
Page 35 and 36: Venkatarao Ganni Director of the MS
Page 37 and 38: Yue Hao Associate Professor of Phys
Page 39 and 40: Morten Hjorth-Jensen Professor of P
Page 41 and 42: Pete Knudsen Senior Cryogenic Proce
Page 43 and 44: Steven Lidia Senior Physicist and A
Page 45 and 46: Steven Lund Professor of Physics Ac
Page 47 and 48: Kei Minamisono Research Senior Phys
Page 49 and 50: Fernando Montes Research Staff Phys
Page 51 and 52: Filomena Nunes Professor of Physics
Page 53 and 54: Peter Ostroumov Professor of Physic
Page 55 and 56: Ryan Ringle Research Senior Physici
Page 57 and 58: Hendrik Schatz University Distingui
Page 59 and 60: Bradley Sherrill University Disting
Page 61 and 62: Artemis Spyrou Professor of Physics
Page 63 and 64: Betty Tsang Professor (FRIB/NSCL) E
Page 65 and 66: Christopher Wrede Associate Profess
Page 67 and 68: Remco Zegers Professor of Physics E
Page 69 and 70: HOW TO APPLY Now that you’ve read

2021FRIB/NSCL Graduate Brochure

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