Calendar

Oct
2
Fri
Colloquium: Rodolfo Montez Jr.
Oct 2 @ 3:15 pm – 4:15 pm
Colloquium: Rodolfo Montez Jr. @ BX102

Insights into Binary Stars, Stellar Winds, and Astrophysical Plasmas from X-ray Observations of Planetary Nebulae

Rodolfo Montez Jr., Vanderbilt University

 

Oct
9
Fri
Colloquium: Ben Weiner
Oct 9 @ 3:15 pm – 4:15 pm
Colloquium:  Ben Weiner @ BX102

Searching for Dwarf Satellites around Milky Way – Analog Galaxies with the SAGA survey

Ben Weiner, Steward Observatory

Dwarf satellites of massive galaxies are a probe of many issues in galaxy evolution and cosmology, including the nature of low-mass galaxies, star formation at early times, accretion into halos, and the abundance of low-mass dark matter halos. Much attention has been devoted to the number and nature of Milky Way and M31 dwarf satellites, especially the “missing satellites problem.” However, we know very little about dwarf satellites outside the Local Group below the mass of the LMC, and we don’t know if the MW and M31 satellite systems are typical. The SAGA (Satellites Around Galactic Analogs) survey collaboration aims to address this with both observational and theoretical studies of satellite abundances and properties around Milky Way analog central galaxies. I will present results from our MMT/Hectospec wide field spectroscopic surveys for satellites. We have surveyed the fields of several nearby galaxies that are similar to the Milky Way to detect and spectroscopically confirm dwarf satellites.  We find a range of numbers of satellites, suggesting that there is a significant variance in halo histories.  We also find that not all dwarf systems resemble the Milky Way and M31 systems. I will discuss these results and some of the implications on the life cycle of satellites that we can infer from satellite abundances and properties, including their images and spectra.

 

Oct
16
Fri
Colloquium: Doug Biesecker
Oct 16 @ 3:15 pm – 4:15 pm
Colloquium: Doug Biesecker @ BX102

Why Space Weather Matters and How Forecasting Will Improve in the DSCOVR Era

Doug Biesecker, NOAA/NWS/Space Weather Prediction Center

Space Weather is a growing enterprise, with growing recognition of its importance inside and outside government.  The largest concern is with the electric power grid, but impacts to Global Positioning Systems (GPS) are also significant.  Other areas of impact include satellites and human space flight, and high frequency communication for aviation, mariners, and emergency responders, among many.  The NOAA National Weather Service’s Space Weather Prediction Center (SWPC) is the nation’s official source of space weather watches, warnings and alerts.  SWPC does this with a 24×7 staffed operation that monitors the Sun, solar wind, and geospace environment taking advantage of a broad suite of observations and models to provide the best forecasts possible.  In conjunction with the growing recognition of space weather, NOAA launched its first mission, the Deep Space Climate Observatory (DSCOVR), out of the Earth’s orbit to an orbit about the L1 Lagrange point.  This is also NOAA’s first satellite mission where space weather is the primary mission and DSCOVR marks the first of what is expected to be a long series of space weather monitoring satellites.  NOAA is also bringing numerical space weather models into the mix of models running on the nation’s supercomputers.  Numerical space weather models have demonstrated the ability to improve the onset time of space weather storms and will, for the first time, allow regional geomagnetic forecasting.  Instead of describing conditions on Earth with a single number, customers will have forecasts tailored to their location.

 

Feb
12
Fri
Colloquium: Lauren Woolsey
Feb 12 @ 3:15 pm – 4:15 pm
Colloquium:  Lauren Woolsey @ BX102

Magnetic Influences on Coronal Heating and the Solar Wind

Lauren Woolsey, Harvard University

 

Abstract

The physical mechanism(s) that generate and accelerate the solar wind have not been conclusively determined after decades of study, though not for lack of possibilities. The long list of proposed processes can be grouped into two main paradigms: 1) models that require the rearranging of magnetic topology through magnetic reconnection in order to release energy and accelerate the wind and 2) models that require the launching of magnetoacoustic and Alfvén waves to propagate along the magnetic field and generate turbulence to heat the corona and accelerate the emanating wind. After a short overview of these paradigms, I will present my ongoing dissertation work that seeks to investigate the latter category of theoretical models and the role that different magnetic field profiles play in the resulting solar wind properties with Alfvén-wave-driven turbulent heating. I will describe the computer modeling in 1D and 3D that I have done of bundles of magnetic field (flux tubes) that are open to the heliosphere, and what our results can tell us about the influences of magnetic field on the solar wind in these flux tubes, including the latest time-dependent modeling that produces bursty, nanoflare-like heating. Additionally, I will present the latest results of our study of chromospheric network jets and the magnetic thresholds we are finding in magnetogram data.

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

Sep
19
Mon
Pizza Lunch: Reta Beebe
Sep 19 @ 12:30 pm – 1:30 pm
Pizza Lunch: Reta Beebe @ AY 119

Title: JUNO

Reta Beebe

A .pdf of the talk can be found here.

 

 

Nov
18
Fri
Colloquium: Karen Olsen
Nov 18 @ 3:15 pm – 4:15 pm
Colloquium: Karen Olsen @ Biology Annex 102

Simulations of the interstellar medium at high redshift: What does [CII] trace?

Dr. Karen Olsen, Arizona State University

We are in an exciting era were simulations on large, cosmological scales meet modeling of the interstellar medium (ISM) on sub-parsec scales. This gives us a way to predict and interpret observations of the ISM, and in particular the star-forming gas, in high-redshift galaxies, useful for ongoing and future ALMA/VLA projects.

In this talk, I will walk you though the current state of simulations targeting the the fine structure line of [CII] at 158 microns, which has now been observed in several z>6 galaxies. [CII] can arise throughout the interstellar medium (ISM), but the brightness of the [CII] line depends strongly on local environment within a galaxy, meaning that the ISM phase dominating the [CII] emission can depend on galaxy type. This complicates the use of [CII] as a tracer of either SFR or ISM mass and calls for detailed modeling following the different ways in which [CII] can be excited.

I will present SÍGAME (Simulator of GAlaxy Millimeter/submillimeter emission) – a novel method for predicting the origin and strength of line emission from galaxies. Our method combines data from cosmological simulations with sub-grid physics that carefully calculates local radiation field strength, pressure, and ionizational/thermal balance. Preliminary results will be shown from recent modeling of [CII] emission from z~6 star-forming galaxies with SÍGAME. We find strong potential for using the total [CII] luminosity to derive the ISM and molecular gas mass of galaxies during the Epoch of Reionization (EoR).