Interests: Remote sensing, Medical diagnostics for space missions

Slides:



Advertisements
Similar presentations
Earth science The study of how the earth changes over time Includes:
Advertisements

The nebular hypothesis
Mantle composition 1800s meteorites contain similar minerals to terrestrial rocks Hypothesis that meteorites come from asteroid belt and originate from.
Geoneutrinos: Earth composition, heat production and deep structures
Solar System Formation – Earth Formation Layers of the Earth Review.
THE CHEMISTRY OF MARS Heather Tennant Earth 438 Presented March 11, 2014.
Anne M. Hofmeister and Robert E. Criss
Mercury’s origin and evolution:- Likely evidence from surface composition David A Rothery 1, J Carpenter 2, G Fraser 2 & the MIXS team 1 Dept of Earth.
Open Questions in Geosciences Collaborators: - Ricardo Arévalo, Mario Luong : UMD - Kevin Wheeler, Dave Walker : Columbia Univ - Corgne, Keshav & Fei :
The other volatile: O 2 What is the mantle/surface/biology connection? Charles H. Langmuir Harvard University
Dust particles and their spectra. Review Ge/Ay 132 Final report Ivan Grudinin.
THE HEAT LOSS OF THE EARTH Claude Jaupart Jean-Claude Mareschal Stéphane Labrosse Institut de Physique du Globe de Paris.
Oxygen Isotope Heterogeneity in the Solar System The Molecular Cloud Origin Hypothesis and its Implications for the Chemical Composition of Meteorites.
Definition of “fossil” A fossil is defined as any remains, trace or imprint of a plant or animal that has been preserved by natural processes in the Earth’s.
Pt. II: Oxygen Isotopes in Meteorites Stefan Schröder February 14, 2006 Lecture Series “Origin of Solar Systems” by Dr. Klaus Jockers.
What have we learned about small bodies and the Solar Nebula over the past 30 years? Joseph Nuth Senior Scientist for Primitive Bodies Solar System Exploration.
A Traveling CAIA Traveling CAI Minerals from a CAI and its prominent rim have a wide range of oxygen.
GEOL3045: Planetary Geology Lysa Chizmadia 16 Jan 2007 The Origin of Our Solar System Lysa Chizmadia 16 Jan 2007 The Origin of Our Solar System.
Planet Earth. Dusty Spiral Galaxy Planetary Science Origin of Earth: Big Bang Relevance to Earth Sciences: Elemental Distribution.
EART160 Planetary Sciences Mikhail Kreslavsky. The Solar System consists of: Stars: –The Sun Planetary bodies  regular shape (~sphere)  layered internal.
Ask the Scientists Questions for Dr. Butner Star Formation 1/29/11.
Astronomy - the study of objects and events in outer space Astronomer - scientist who studies astronomy.
Nebulae. “Nebula” comes from the Latin word for cloud. “Nebulae” is the plural. It is loosely applied to anything that looks fuzzy or extended in a telescope.
The Universe Science 8.
Isotopic constraints on nucleosynthesis, Solar System composition & accretion Nikitha Susan Saji Centre for Star and Planet Formation, Natural History.
Comparative global energy budgets for Earth, Mars and Venus P. L. Read, S. Chelvaniththilan, P. G. J. Irwin, S. Knight, S. R. Lewis, J. Mendonça, L. Montabone.
The Early Earth “Mr. Montgomery’s Early Earth PowerPoint redefines PowerPoint excellency” - PPTA.
Formation of Our Solar System
永島一秀, 小林幸雄, 坂本直哉, 殿谷梓, 圦本尚義 東工大・地球惑星科学 Presolar Silicates in meteorites Presolar Silicates in Primitive Chondrites Mar. 02, 2005 K. Nagashima, S. Kobayashi,
In the beginning… The composition of the solar system and earth.
SIO224 Internal Constitution of the Earth Fundamental problem: the nature of mass and heat transfer in the mantle and the evolution of the Earth.
Why measure Geoneutrinos: the Earth's Heat Budget
A new look at lower mantle structure through cluster analysis Ved Lekic CIDER post-AGU workshop 2011.
What makes up the Solar System and what force is holding it in place? The Force of Gravity hold our Solar System in Place. Things that make up our Solar.
GALAXY Photo credit: SEDS Messier Catalogue – M51.
The Core and Mantle: future prospects for understanding the Deep Earth
How do habitable planets acquire carbon? PAHs in Protoplanetary Disks
Brief history of the universe. Atoms Atoms – consist of a dense nucleus of positively charged protons and uncharged neutrons surrounded by a cloud of.
Importance of tighter constraints on U and Th abundances of the whole Earth by Geo-neutrino determinations Shun’ichi Nakai ERI, The University of Tokyo.
Nucleosynthetic processes: Fusion: Hydrogen Helium Carbon Oxygen After Fe, neutron addition takes place (rapid and slow processes)
Origin of the solar system Solar Systems Form by Accretion.
Jeff Taylor Course Introduction1 GG 673C: Petrologic Evolution of the Moon and Mars Course Introduction Why the Moon and Mars?
1.3 notes  There are 3 types of heat transfer: radiation, conduction, and convection.  The transfer of energy through space is radiation. Sunlight.
The Formation and Structure of Planet Earth Lesson #1: The Infant Earth Lesson Objective #1.
Leah Salditch February 27, 2017 Mars Final Project
Orbital Evolution of Dust Grains and Rocks During FU Orionis Outbursts
Origin of the solar system Solar Systems Form by Accretion Let us study the sequence in slightly more detail: The processes by which.
Pt. II: Oxygen Isotopes in Meteorites
Savage et al. Copper isotope evidence for large-scale sulphide fractionation during Earth’s differentiation Figure 2 Schematic evolution of Cu concentration.
Temperature, Heat, and the First Law of Thermodynamics
SIO224 Internal Constitution of the Earth
The Universe in the Infrared
Water in Asteroid 4 Vesta
A Traveling CAI Overview: Calcium-aluminum-rich inclusions (CAIs) are the oldest solids to form in the Solar System. They occur in every type of chondrite,
Galaxies, Stars, and Planets Oh My!
Meteoroids, Asteroids Dwarf Planets
NGC 1068 Torus Emission Turn-over
Dating Transient Heating Events in the Solar Protoplanetary Disk
[CII] observations of the Ring nebula (NGC 6720)
Mid-IR spectroscopic observations of
Vocabulary Week 3-4 Sustaining Life.
Meteoroids, Asteroids Dwarf Planets
[CII] observations of the Ring nebula (NGC 6720)
Origin of 17,18O-rich materials from Acfer 094
No gum, candy or chewing please! 
Planetary Geology: dominant processes
VNGS science highlight: PDR models of M51
Eventually, the star's fuel will begin to run out
Low hydrogen contents in the cores of terrestrial planets
Meteoroids, Asteroids Dwarf Planets
Presentation transcript:

Interests: Remote sensing, Medical diagnostics for space missions

Hofmeister’s research: Combine measurements of spectra, heat transfer, and thermal expansivity with other available data and basic physical principles to understand processes from microscopic to grand scales. Stars, Dust and Nebula in NGC 6559 Credit: Jean-Charles Cuillandre (CFHT)

Planets and Stars form from collapse of dusty clouds: R.E. = ½Iw2 Star data: M35: Meibom et al. (2009) ApJ, 695, 679-694 M50: Irwin et al. (2009) MNRAS, 392, 1456-1466 Hofmeister and Criss: 2012 Planetary and Space Science 62, p. 111-131.

Earth’s composition from its radiogenic emissions and meteorite data Chondrites  Upper mantle Silicates Oxygen isotopes of meteorites require two reservoirs Bulk Oxide Earth CAIs  Lower mantle Hofmeister and Criss (2013) Gondwana Research 24, p. 490–500