|Professor of Physics|
Ph.D. 1971, Princeton
B.A. 1968, California (Berkeley)
Theoretical Particle Physics, Astrophysics and Cosmology
|Email:||gf25 AT nyu.edu|
|Personal Home Page:||http://cosmo.nyu.edu/~gf25/|
Prof. Glennys Farrar received her Ph. D. in theoretical physics from Princeton University in 1971, breaking the gender-barrier in physics at Princeton in the process. She was a member of the Institute for Advanced Study and on the faculties of the California Institute of Technology and Rutgers University before moving to NYU in 1998. Among her accomplishments in particle physics, Farrar is perhaps best known for pioneering the phenomenological study of supersymmetry. With P. Fayet and others, she developed most of the present search techniques for superparticles, gave the first limits on SUSY breaking and superpartner masses from accelerator experiments and precision observables such as g-2, identified and clarified the role of R-parity, initiated the study of cosmological effects of SUSY. She has stressed the interest of light gaugino scenarios and has lead the effort to constrain them from experiment. Her other work has ranged from QCD and hadron physics to electroweak baryogenesis and the study of dark matter. She made a number of predictions whose experimental confirmation played an important role in establishing the Standard Model. The scaling dependence of exclusive scattering was the first clear demonstration that quarks are dynamical degrees of freedom, and not merely a mathematical device realizing current algebras. Other predictions which play an important role in QCD phenomenology today include copious direct production of photons in hadronic collisions, the ratio of up to down quarks and the dependence of quark and gluon distributions at large x-Bjorken, color-transparency, the normalization of the pion form wavefunction, and helicity dependence of hadron scattering.
Farrar's current work focuses mainly on problems at the intersection of astrophysics, cosmology and particle physics, including ultrahigh energy cosmic rays, the nature of dark matter and dark energy, and the origin of the asymmetry between matter and antimatter. UHECRs: Farrar and collaborators use existing UHECR data to deduce properties of their sources and cosmic magnetic fields. Another thrust of NYU research is to improve simulation and reconstruction of cosmic ray air showers. H. Drescher, a postdoc in Farrar's group, developed the shower simulation code SENECA; it gives a more realistic description of individual events and is 40 times faster than previous codes. Farrar and Drescher have used it to check the reliability and model independence of UHECR energy calibrations; with Courant grad student D. Krasnov, more powerful methods to identify and reconstruct a primary cosmic ray's energy are being developed. Dark Matter and Cosmological Dynamics: Farrar and Peebles showed the mass of dark matter could arise from a Higgs-type interaction with the dark energy field, producing interesting variants to the standard LCDM cosmological model. Farrar is now engaged in several related projects, simulating the impact of such interactions on the formation of structure and using observations of large-scale structure and galactic dynamics to constrain the possibility that dark matter experiences non-gravitational forces. Novel models of Dark Matter: Farrar and Spergel are studying models in which DM is normal matter on a different brane. Farrar and grad student G. Zaharijas have shown that the baryon asymmetry of the universe may be only an asymmetry in "packaging", with the baryon number in nucleons balanced by anti-baryonic dark matter. Observational constraints on such DM have been obtained and are found to be consistent with the expected DM properties. In one such scenario the DM consists of H and anti-H dibaryons, impelling a renewed study of a long-lived H dibaryon.
|THE 2DF GALAXY REDSHIFT SURVEY: LUMINOSITY FUNCTIONS BY DENSITY ENVIRONMENT AND GALAXY with the 2dFGRS Collaboration (Darren J. Croton et al.). Jul 2004. 14pp. Submitted to Mon.Not.Roy.Astron.Soc. e-Print Archive: astro-ph/0407537 link to the document|