Calendar

Mar
7
Mon
Pizza Lunch: Ofelia Ruiz and Lorenza Sanchez
Mar 7 @ 12:30 pm – 1:30 pm
Pizza Lunch: Ofelia Ruiz and Lorenza Sanchez @ AY 119

Making your life easier: Overview of NMSU policies and procedures. Things you can do to speed up payments/forms through the system

Ofelia Ruiz and Lorenza Sanchez

 

Apr
8
Fri
Colloquium PhD Defense: Meredith Rawls
Apr 8 @ 3:00 pm – 4:00 pm
Colloquium PhD Defense: Meredith Rawls @ BX102

Red Giants in Eclipsing Binaries as a Benchmark for Asteroseismology

Meredith Rawls, NMSU

Apr
18
Mon
Pizza Lunch: Sam Schonfeld
Apr 18 @ 12:30 pm – 1:30 pm
Pizza Lunch: Sam Schonfeld @ AY 119

Title: Investigating the temporal evolution of the solar F10.7 radio flux

Sam Schonfeld

 

Apr
25
Mon
Pizza Lunch: Jeremy Emmett 598
Apr 25 @ 12:30 pm – 1:30 pm
Pizza Lunch: Jeremy Emmett 598 @ AY 119

Title: Jeremy Emmett 598

Name

 

May
2
Mon
Pizza Lunch: Agnar Hall 598
May 2 @ 12:30 pm – 1:30 pm
May
9
Mon
Pizza Lunch: Laurel Farris 598
May 9 @ 12:30 pm – 1:30 pm
Pizza Lunch: Laurel Farris 598

Laurel Farris 598

May
12
Thu
Colloquium PhD Defense: Kenz Arraki
May 12 @ 3:00 pm – 4:00 pm
Colloquium PhD Defense: Kenz Arraki @ Dominici106

Evolution of Dwarf Galaxy Properties in Local Group Environments

Kenz Arraki, NMSU

May
31
Tue
Colloquium PhD Defense: Diane Feuillet
May 31 @ 3:00 pm – 4:00 pm
Colloquium PhD Defense: Diane Feuillet @ Dominici106

Ages and Abundance of Local Stellar Populations

Diane Feuillet, NMSU

Mar
13
Mon
Pizza Lunch: Jean McKeever
Mar 13 @ 12:30 pm – 1:30 pm
Pizza Lunch: Jean McKeever @ AY 119

Red Giants in Eclipsing Binary Systems

Jean McKeever

 

Sep
20
Wed
Colloquium PhD Defense: Jean McKeever
Sep 20 @ 3:00 pm – 4:15 pm
Colloquium PhD Defense: Jean McKeever @ Business College 103

Asteroseismology of Red Giants: The Detailed Modeling of Red Giants in Eclipsing Binary Systems

Jean McKeever, NMSU

Asteroseismology is an invaluable tool that allows one to peer into the inside of a star and know its fundamental stellar properties with relative ease. There has been much exploration of solar-like oscillations within red giants with recent advances in technology, leading to new innovations in observing. The Kepler mission, with its 4-year observations of a single patch of sky, has opened the floodgates on asteroseismic studies. Binary star systems are also an invaluable tool for their ability to provide independent constraints on fundamental stellar parameters such as mass and radius. The asteroseismic scaling laws link observables in the light curves of stars to the physical parameters in the star, providing a unique tool to study large populations of stars quite easily. In this work we present our 4-year radial velocity observing program to provide accurate dynamical masses for 16 red giants in eclipsing binary systems. From this we find that asteroseismology overestimates the mass and radius of red giants by 15% and 5% respectively. We further attempt to model the pulsations of a few of these stars using stellar evolution and oscillation codes. The goal is to determine which masses are correct and if there is a physical cause for the discrepancy in asteroseismic masses. We find there are many challenges to modeling evolved stars such as red giants and we address a few of the major concerns. These systems are some of the best studied systems to date and further exploration of their asteroseismic mysteries is inevitable.