<html><body><div style="font-family: arial, helvetica, sans-serif; font-size: 12pt; color: #000000"><div><p style="text-align: center; border: medium none; padding: 0in; margin: 0px;" data-mce-style="text-align: center; padding: 0in; margin: 0px;"><strong><span style="font-size: 48.0pt; line-height: 107%; font-family: 'Times New Roman',serif;" data-mce-style="font-size: 48.0pt; line-height: 107%; font-family: 'Times New Roman',serif;">Physics Seminar</span></strong></p><p style="margin: 0px; text-align: center; line-height: normal;" data-mce-style="margin: 0px; text-align: center; line-height: normal;"><strong><span style="font-size: 16.0pt; font-family: 'Times New Roman',serif;" data-mce-style="font-size: 16.0pt; font-family: 'Times New Roman',serif;">Farrooh Fattoyev</span></strong></p><p style="margin: 0px; text-align: center; line-height: normal;" data-mce-style="margin: 0px; text-align: center; line-height: normal;"><strong><span style="font-size: 16.0pt; font-family: 'Times New Roman',serif;" data-mce-style="font-size: 16.0pt; font-family: 'Times New Roman',serif;">Indiana University, Bloomington</span></strong></p><p style="margin: 0px;" data-mce-style="margin: 0px;"> </p><p style="text-align: center; margin: 0px;" data-mce-style="text-align: center; margin: 0px;"><em><span style="font-size: 18.0pt; line-height: 107%; font-family: 'Times New Roman',serif;" data-mce-style="font-size: 18.0pt; line-height: 107%; font-family: 'Times New Roman',serif;">Connecting Neutron Skins to Gravitational Waves<br> <br> </span></em></p><p style="text-align: center; margin: 0px;" data-mce-style="text-align: center; margin: 0px;"><span><strong><span style="font-size: 16.0pt; line-height: 107%; font-family: 'Times New Roman',serif;" data-mce-style="font-size: 16.0pt; line-height: 107%; font-family: 'Times New Roman',serif;">Abstract</span></strong></span><strong><span style="font-size: 16.0pt; line-height: 107%; font-family: 'Times New Roman',serif;" data-mce-style="font-size: 16.0pt; line-height: 107%; font-family: 'Times New Roman',serif;">:</span></strong></p><p style="text-align: justify; margin: 0px;" data-mce-style="text-align: justify; margin: 0px;"><br> <br> <span style="font-size: 12.0pt; line-height: 107%;" data-mce-style="font-size: 12.0pt; line-height: 107%;">The historical first detection of a binary neutron star (BNS) merger by the LIGO-Virgo collaboration is providing fundamental new insights into the nature of dense neutron-rich nuclear matter. By using a set of realistic models of the equation of state (EOS) that yield an accurate description of the properties of finite nuclei, support neutron stars of two solar masses, and provide a Lorentz covariant extrapolation to dense matter we confront their predictions against the measured tidal deformability from the BNS merger. These models also predict a range of neutron skin thicknesses in Pb-208 that is consistent with the lower-to-central values of the first model-independent measurement of the neutron skin by the PREX Collaboration, i.e. 0.15 fm ≤ R_skin ≤ 0.33 fm. Since the gravitational-wave signal is sensitive to the underlying EOS, limits on the tidal deformability inferred from the observation translate into constraints on the neutron-star radius. In particular, we find an upper limit on the radius of a 1.4 solar-mass neutron star of R < 13.76 km. And given the sensitivity of the neutron-skin thickness of Pb-208 to the density dependence of the symmetry energy, hence to the neutron star radii, we infer a corresponding upper limit on the neutron skin of about R_skin </span><span style="font-size: 12.0pt; line-height: 107%; font-family: 'Cambria Math',serif;" data-mce-style="font-size: 12.0pt; line-height: 107%; font-family: 'Cambria Math',serif;">≲</span><span style="font-size: 12.0pt; line-height: 107%;" data-mce-style="font-size: 12.0pt; line-height: 107%;"> 0.25 fm. If the upcoming PREX-II (or CREX) experiment measures a significantly thicker skin in Pb-208 (or in Ca-48 as predicted by the same models), this may be evidence of a softening of the symmetry energy at high densities – likely indicative of a phase transition in the interior of neutron stars.</span></p><p style="text-align: justify; margin: 0px;" data-mce-style="text-align: justify; margin: 0px;"><span style="font-size: 12.0pt; line-height: 107%; font-family: 'Times New Roman',serif;" data-mce-style="font-size: 12.0pt; line-height: 107%; font-family: 'Times New Roman',serif;"> </span></p><p style="text-align: center; margin: 0px;" data-mce-style="text-align: center; margin: 0px;"><strong><span style="font-size: 18.0pt; line-height: 107%; font-family: 'Times New Roman',serif;" data-mce-style="font-size: 18.0pt; line-height: 107%; font-family: 'Times New Roman',serif;">Wednesday January 24, 2018</span></strong></p><p style="text-align: center; margin: 0px;" data-mce-style="text-align: center; margin: 0px;"><strong><span style="font-size: 18.0pt; line-height: 107%; font-family: 'Times New Roman',serif;" data-mce-style="font-size: 18.0pt; line-height: 107%; font-family: 'Times New Roman',serif;">11:00am</span></strong></p><p style="text-align: center; margin: 0px;" data-mce-style="text-align: center; margin: 0px;"><strong><span style="font-size: 18.0pt; line-height: 107%; font-family: 'Times New Roman',serif;" data-mce-style="font-size: 18.0pt; line-height: 107%; font-family: 'Times New Roman',serif;">CEBAF F113</span></strong></p></div><div><br></div><div data-marker="__SIG_POST__">-- <br></div><div>Stephanie Tysor<br>Hall A Administrative Assistant<br>Thomas Jefferson National Accelerator Facility<br>(office)757-269-6005 (fax)757-269-5235</div></div></body></html>