Other Seminars

Artist’s conception of early Earth.

The Earth is about 4.5 billion years old, and it’s seen some dramatic events during that time – from the giant Moon-forming impact to the advent of fidget spinners.

The earliest phase in the Earth’s history, called the Hadean, was hellish. During long stretches, the surface was probably molten, the atmosphere was toxic, and there were no oceans. Eventually, though, the Earth transitioned to its current hospitable condition, and life got a toehold by at least 3.5 billion years ago.

But today in the Boise State Geosciences seminar, we heard about possible evidence for life going back almost a billion years earlier from Dr. Elisabeth Bell of UCLA’s Earth, Planetary, and Space Sciences Dept.

Optical microscope photograph; the length of the crystal is about 250 µm.

Dr. Bell’s work focuses on the hardiest of all mineral grains, the mighty zircons. These little rocks can be smaller than the width of a human hair, but they provide some of the strongest clues about conditions on the early Earth.

The mineral from which they’re made is very tough, and so weathering processes that usually break down other minerals barely affect zircons at all. Consequently, zircons that formed billions of years ago still retain their integrity, and, like the amber from “Jurassic Park”, often contain treasures in the form of other minerals. Dr. Bell and her team analyze these mineral time-capsules to learn what the early Earth was like.

One of the most exciting finds from her work comes from the Jack Hills geological formation in western Australia, where rocks almost as old as the Earth can be found. Inside these rocks are even older zircons, dating back to 4.1 billion years ago, which themselves have trapped small grains of graphite.

By analyzing the isotopic composition of these graphite grains, Dr. Bell has found tantalizing evidence for chemical processing of carbon that resembles biology. Although the evidence is still tentative, the results suggest life on Earth started chugging away smack in the middle of the Hadean, much earlier than has previously been believed.

Taking a step back, such a result suggests that life may get started on an Earth-like planet very quickly, which could mean that life is an almost inevitable outcome of the evolution of Earth-like planets. Given how common Earth-like planets may be, that could mean the universe may be replete with at least simple life.

Illustration of tidal interactions. From ftp://ftp.osupytheas.fr/pub/symposiumCOROT/posters/Francoise-Remus-Poster.pdf.

Illustration of tidal interactions. From ftp://ftp.osupytheas.fr/pub/symposiumCOROT/posters/Francoise-Remus-Poster.pdf.

I attended a talk at the US Naval Observatory on Friday given by newly minted Dr. Françoise Remus of the Paris Observatory. Remus discussed tidal interactions between the Jovian or giant planets and their satellites.

Tides are well known here on Earth, where the Moon raises tides in the oceans on a regular basis, as seen in the Chesapeake Bay. The moons of Jupiter and Saturn also raise tides on those planets, in the planets’ atmospheres and deep interiors.

The tides raised on these planets interact gravitationally with the satellites and influence the moons’ orbits, as for the Earth’s Moon — tides on the Earth push the Moon away from the Earth a few centimeters every year.

On Earth, drag in the oceans provides tidal dissipation that drives the Moon’s orbital evolution. Tides raised on Jupiter and Saturn apparently also experience dissipation, but since those planets don’t have shallow oceans, it’s not clear what generates the dissipation.

For her graduate work, Remus created complex models to explain tidal dissipation within Jupiter and Saturn and showed that the planets’ rocky and icy cores, deep within their interiors, play a key and previously under-appreciated role. Her work has broad implications, from helping us understand these planets’ mysterious interiors to explaining the origins of the planets’ complex satellite systems.

This natural color composite was taken during the Cassini spacecraft's April 16, 2005, flyby of Titan. From http://en.wikipedia.org/wiki/Titan_%28moon%29.

This natural color composite was taken during the Cassini spacecraft’s April 16, 2005, flyby of Titan. From http://en.wikipedia.org/wiki/Titan_%28moon%29.

Interesting public talk to the National Capital Astronomers‘ monthly meeting from Prof. Doug Hamilton of UMD Astronomy.

Prof. Hamilton talked about the origin of Saturn’s moon Titan, an unusual satellite in several ways. Titan has a massive nitrogen and methane atmosphere, full of orange photochemical haze (picture at left).

Prof. Hamilton pointed out that that Saturn’s satellite system is also unique among satellite systems of giant planets: unlike the Jovian and Uranian systems, Titan is the only large moon, and it is very far from the next largest moons in the system.

Instead of forming along with its host planet, as the Jovian and Uranian satellites probably did, Prof. Hamilton suggested that several smaller satellites originally formed around Saturn. Then the moons’ orbits destabilized, and the moons collided, merging to form Titan.

This novel hypothesis solves several outstanding questions about Titan and highlights how much we still don’t understand about our own solar system.

This is an enlarged image of the region around the Kleinman-Low nebula in the Orion cloud located 1500 light years away. This image is taken in light at 2.12 micron at the Subaru telescope, which is emitted by warm molecular hydrogen gas with an absolute temperature of 2000 K.

This is an enlarged image of the region around the Kleinman-Low nebula in the Orion cloud located 1500 light years away, where a massive star may be in the process of forming. This image was taken in light at 2.12 micron at the Subaru telescope, which is emitted by warm molecular hydrogen gas with an absolute temperature of 2000 K.

I saw an interesting colloquium talk today at the National Radio Astronomy Observatory, given by Prof. Jonathan Tan about formation of massive stars.

Many details about the formation process for massive stars remain unclear, and Prof. Tan described that the stars may either form through the merger of many small, low-mass stellar cores or by direct accretion of massive quantities of gas.

And big questions about these processes remain. For example, what spurs the initial collapse of a gas cloud into star? How exactly is the mass accreted, and what forces dominate that accretion? How long do all these processes take?

Prof. Tan described observations of clumps of gas and dust in the galaxy, including observations from the world’s largest radio telescope, the ALMA array, and how these observations may provide constraints on the star formation processes.