Calendar

Nov
17
Tue
ASTR 605 – The Interstellar Medium today
Nov 17 @ 8:55 am – 10:10 am
Nov
18
Wed
ASTR 575 – Computational Astrophysics
Nov 18 @ 9:00 am – 10:15 am
Nov
19
Thu
ASTR 605 – The Interstellar Medium today
Nov 19 @ 8:55 am – 10:10 am
Nov
30
Mon
ASTR 575 – Computational Astrophysics
Nov 30 @ 9:00 am – 10:15 am
Dec
1
Tue
ASTR 605 – The Interstellar Medium today
Dec 1 @ 8:55 am – 10:10 am
Dec
2
Wed
ASTR 575 – Computational Astrophysics
Dec 2 @ 9:00 am – 10:15 am
Dec
3
Thu
ASTR 605 – The Interstellar Medium today
Dec 3 @ 8:55 am – 10:10 am
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

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

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.