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<p style="margin:0in"><span style="font-family:"Cambria",serif;color:black">( A PDF attached)<o:p></o:p></span></p>
<p class="MsoNormal" align="center" style="text-align:center"><b><span style="font-size:28.0pt;font-family:"Cambria",serif;color:#C00000">Fall 2021 Colloquium</span></b><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p></o:p></span></p>
<p class="MsoNormal" align="center" style="text-align:center"><b><span style="font-size:16.0pt;font-family:"Cambria",serif;color:black">Department of Physics & Astronomy, A&M-Commerce</span></b><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p></o:p></span></p>
<p class="MsoNormal" align="center" style="text-align:center"><b><span style="font-size:16.0pt;font-family:"Cambria",serif;color:#C00000">Nov 11, Thursday, 4-5 PM</span></b><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p></o:p></span></p>
<p class="MsoNormal" align="center" style="text-align:center"><b><span style="font-size:14.0pt;font-family:"Cambria",serif;color:black">Live Zoom Meeting</span></b><span style="font-size:14.0pt;font-family:"Cambria",serif;color:black"><br>
</span><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><a href="https://tamuc.zoom.us/j/99681875042"><span style="font-family:"Cambria",serif;color:#1155CC">https://tamuc.zoom.us/j/99681875042</span></a><o:p></o:p></span></p>
<p class="MsoNormal" align="center" style="text-align:center"><span style="font-size:11.0pt;font-family:"Cambria",serif;color:black">Meeting ID: 996 8187 5042</span><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p></o:p></span></p>
<p class="MsoNormal" align="center" style="text-align:center"><b><span style="font-size:14.0pt;font-family:"Cambria",serif;color:#00B050">Nuclear Physics</span></b><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p></o:p></span></p>
<p class="MsoNormal" align="center" style="text-align:center"><b><span style="font-size:18.0pt;font-family:"Cambria",serif;color:blue">The CNO cycle and the CNO Neutrinos in our Sun<br>
</span></b><b><span style="font-size:14.0pt;font-family:"Cambria",serif;color:black">Dr. Michael Wiescher</span></b><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p></o:p></span></p>
<p class="MsoNormal" align="center" style="text-align:center"><b><span style="font-size:14.0pt;font-family:"Cambria",serif;color:#0B5394">University of Notre Dame</span></b><b><span style="font-size:14.0pt;font-family:"Cambria",serif;color:black"> </span></b><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p></o:p></span></p>
<p class="MsoNormal" align="center" style="text-align:center"><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><br>
<span style="border:none windowtext 1.0pt;padding:0in"><img border="0" width="144" height="144" style="width:1.5in;height:1.5in" id="Picture_x0020_2" src="cid:image003.jpg@01D7D546.06EFBA00"></span><o:p></o:p></span></p>
<p class="MsoNormal" align="center" style="text-align:center"><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p> </o:p></span></p>
<p class="MsoNormal" style="text-align:justify;text-justify:inter-ideograph"><span style="font-size:11.0pt;font-family:"Arial",sans-serif;color:black">Dr. Michael Wischer received a Ph.D. degree (1980) in Physics at the Universität Münster, Germany. He worked
as a postdoc at Ohio State University and CalTech between 1980 and 1984, and as a senior researcher at Universität Mainz Germany until 1986. Dr. Wiescher began his appointment as an assistant professor at the University of Nortre Dame in 1986, where he is
currently doing research in nuclear physics as a full professor. More information can be found at
</span><span style="font-size:10.0pt;font-family:"Arial",sans-serif;color:black"><br>
</span><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><a href="https://physics.nd.edu/people/faculty/michael-wiescher/"><span style="font-size:10.0pt;font-family:"Arial",sans-serif;color:#1155CC">https://physics.nd.edu/people/faculty/michael-wiescher/</span></a><o:p></o:p></span></p>
<p class="MsoNormal"><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p> </o:p></span></p>
<p class="MsoNormal"><b><span style="font-size:14.0pt;font-family:"Cambria",serif;color:black">Abstract</span></b><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p></o:p></span></p>
<p class="MsoNormal" style="margin-bottom:12.0pt;text-align:justify;text-justify:inter-ideograph">
<span style="font-size:11.0pt;font-family:"Arial",sans-serif;color:black">The origin of the solar neutrinos is typically associated with the mechanism of our sun converting four hydrogen nuclei hydrogen to helium while converting two protons into neutrons
by a weak interaction process. The discrepancies between neutrino observation and prediction was known for years as the solar neutrino problem in nuclear astrophysics. With the confirmation of neutrino oscillations the solar neutrino problem is considered
to be solved and neutrinos offer a unique tool for observing the interior of the sun. The bulk of the solar neutrinos are originated in the pp-chains which carry more than 97 % of the energy production of the sun, the remaining energy comes from the catalytic
CNO cycles, which dominate the hydrogen burning of more massive stars. The CNO cycles are associated with the origin of the CNO neutrinos from the β-decay of
</span><sup><span style="font-size:6.5pt;font-family:"Arial",sans-serif;color:black">13</span></sup><span style="font-size:11.0pt;font-family:"Arial",sans-serif;color:black">N,
</span><sup><span style="font-size:6.5pt;font-family:"Arial",sans-serif;color:black">15</span></sup><span style="font-size:11.0pt;font-family:"Arial",sans-serif;color:black">O in the first CNO cycle. The observation of these neutrinos would provide a direct
way of measuring the metallicity (or CNO abundances) in our sun, addressing the present discrepancies between the spectroscopic results from surface studies and predictions from helioseismology, which should agree with each other in the framework of the standard
solar model. A critical parameter for these studies are the reaction rates of </span>
<sup><span style="font-size:6.5pt;font-family:"Arial",sans-serif;color:black">12</span></sup><span style="font-size:11.0pt;font-family:"Arial",sans-serif;color:black">C(p,γ)</span><sup><span style="font-size:6.5pt;font-family:"Arial",sans-serif;color:black">13</span></sup><span style="font-size:11.0pt;font-family:"Arial",sans-serif;color:black">N
and </span><sup><span style="font-size:6.5pt;font-family:"Arial",sans-serif;color:black">14</span></sup><span style="font-size:11.0pt;font-family:"Arial",sans-serif;color:black">N(p,γ)</span><sup><span style="font-size:6.5pt;font-family:"Arial",sans-serif;color:black">15</span></sup><span style="font-size:11.0pt;font-family:"Arial",sans-serif;color:black">O
at solar temperatures. I will discuss new experimental studies to determine these rates and remove the still existent uncertainties that affect the CNO abundance predictions of the standard solar model.</span><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p></o:p></span></p>
<p style="margin:0in"><span style="font-size:11.0pt;font-family:"Calibri",sans-serif"><o:p> </o:p></span></p>
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