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Events on Tuesday, March 14th, 2023

Academic Calendar
Spring recess
Abstract: *Note: actual end time may vary.* URL:
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Dept potluck
Spring break potluck lunch/Pi Day
Time: 12:00 pm - 1:30 pm
Place: 4274 Chamberlin
Speaker: Sharon Kahn
Abstract: Join in for a potluck lunch during spring break. . . and let’s celebrate Pi Day at the same time! Here are the details: When: Tues, March 14 (3/14), 12-1:30pm Where: 4274 CH What to bring: Bring a dish to share – and let’s celebrate the diversity of cultures and backgrounds in our department – we encourage you to bring something yummy from your culture. Given that it’s also Pi Day – feel free to bring pie. . .or just something round! How do I sign up: Sign up ( to let us know who is coming and what you think you’ll bring. Who: Any and all Physics folks (grads, faculty, staff, postdocs, undergrads) The department will provide plates and eating utensils. We also have a variety of serving spoons/tongs, if needed. The department will also provide soda and sparkling water. Questions? Ask Sharon or Elizabeth or Evan or Leigh
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Theory Seminar (High Energy/Cosmology)
Recent Progress of String Lamppost Principle
Time: 4:00 pm - 5:15 pm
Place: Chamberlin 5280
Speaker: Yuta Hamada, KEK
Abstract: The String Lamppost Principle (or String Universality) is the statement that all consistent gravitational EFT are obtained as vacua of string theory. In this talk, I first introduce the Swampland Conjectures and discuss how the String Lamppost Principle can be explained by using the brane probes.
Host: Gary Shiu
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Network in Neutrinos, Nuclear Astrophysics, and Symmetries (N3AS) Seminar
Neutron star mass and radius constrained from the magnetar QPOs
Time: 6:00 pm
Place: Join Zoom Meeting Meeting ID: 912 3071 4547
Speaker: Hajime Sotani
Abstract: Quasi-periodic oscillations (QPOs) observed in giant flare from the magnetar, which is a strongly magnetized neutron star, are crucial information for extracting the neutron star properties. To theoretically explain the QPOs newly observed in GRB 200415A, we systematically examine the crustal torsional oscillations. Then, we find that the observed QPOs can be identified with several overtones of crustal oscillations, if the value of the combination of the nuclear saturation parameters, $\varsigma$, is well-selected, depending on the neutron star mass and radius. Thus, we can inversely constrain the neutron star mass and radius for GRB 200415A by comparing to the appropriate range of $\varsigma$ expected with the fiducial value of nuclear saturation parameters obtained from the terrestrial experiments. We further make the neutron star mass and radius constraint more severe by assuming that the neutron star radius is almost the same as that for the neutron star model, whose central density is twice the nuclear saturation density. The resultant neutron star models are consistent with the constraints obtained from the other astronomical and experimental observations.
** Please note the special time of 6 PM CDT **
Host: A. Baha Balantekin
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