11/07/2002
An Anemic Star
Last week, when I mentioned casting my first vote for Dwight Eisenhower, I didn''t realize that this week marks the 50th anniversary of that vote and of moving with my family to New Jersey. If I hadn''t read the November/December American Heritage, these personal milestones would have passed me by unnoticed. I also forgot that November 1 marked the 50th anniversary of a truly earthshaking event, the explosion of the first hydrogen bomb on an island in the Pacific Ocean. That poor little island was obliterated in the explosion.
While the atom bombs dropped on Japan were awesome in their destructive effects, the hydrogen bomb was a thousand times more powerful. The atom bomb utilized nuclear fission, the splitting up of atoms, while the hydrogen bomb employed nuclear fusion, the fusing of atoms. The fusing of hydrogen atoms {actually, protons) to form helium fuels our sun and the stars and leads us to our topic this week. I haven''t written about stars for a while but regular readers will know that I can''t resist space-related topics for long. Take the newspaper article by Rick Callahan headlined "Astronomers discover a star of the ''Class of 13 Billion B.C.''" that I saw last week in our Star Ledger.
The news article was based on a report by Norbert Christlieb and 8 co-authors that appeared in the October 31 issue of Nature. Christlieb, a 36-year old assistant professor at Hamburger Sternwarte in Hamburg, Germany has a good sense of humor. A picture on his Web site shows him with his feet propped up on a desk, which has two computer monitors and an open notebook. Yet the caption assures us that this is not a picture of him at work, but of him on his last holiday on La Palma island. Another picture shows him smiling broadly, holding an overhead projector with the lamp section of the projector covering his upper face like a mask. I found Christlieb to be a kindred soul. He follows up giving his e-mail address with his wish that all bulk e-mail senders end up in hell! (I just finished deleting, without reading, 34 bulk e-mail messages I received today!)
But I digress. Let''s get back to "The class of 13 Billion B.C.", so termed by George C. Preston, retired director of the Carnegie Observatories in Pasadena, California. To appreciate the significance of the work of Christlieb and his colleagues, we have to go back to my favorite subject, the Big Bang. You may recall that after the Bang there were no stars for quite a long time. Finally, stars began to form. However, way back then there was only hydrogen, some helium and a tad of lithium from which to form these stars. In those early days, there weren''t any metallic elements around.
So, how did the metallic elements like iron, for example, come into being? They were formed in the interior of the stars where all that fusion was going on, forming heavier and heavier elements. When the bigger stars blew up as supernova, these monumental explosions flung the iron and other heavy elements out into the universe where new generations of stars were formed. These new stars started out with some of that iron and other heavy elements. As more generations of stars blew up and new ones formed, the newer stars became richer and richer in iron and the other heavy elements. Our sun is a relative youngster as stars go, having formed only about 5 billion years ago.
If this scenario is correct, one might hope to be able to look back into time via a telescope and see light from that first generation of stars formed 12 to 13 billion years ago. These earliest stars should have a lot less iron in them than the stars of our present day universe such as our sun. To actually see individual stars as they were 12 billion years ago is asking a lot from our modern telescopes, even as sophisticated as they are. What about the possibility that there are nearby stars that formed in those earliest of times and haven''t blown up or burned out? About 25 years ago, astronomers did indeed find stars having 10,000 times less iron than in our sun.
But some people are never satisfied. Christlieb and his ilk have been trying to find stars of an even earlier vintage and now report that they have found a star that is more than 12 billion years old. This star has 200,000 times less iron than we find on the sun and is thought to be a star formed from the debris of one of the very first generation stars. What''s more, this star, quaintly named HE0107-5240, is practically next door. It''s only 36,000 light years away, near the center of our own Milky Way galaxy. The hope is that such stars can help to reveal the composition of the pristine gas resulting from the Big Bang.
How much iron is in our own star, the sun? Not having this figure at my fingertips, I searched the Web and found on the University of Tennessee, Knoxville site that the sun is 73% by weight hydrogen and 25% helium, with iron weighing in at a mere 0.14%. Other sources are roughly in agreement with these figures. However, I was intrigued by a host of references on the Web to "iron sun". When they weren''t related to a musical group of some sort, these iron sun references concerned one Oliver Manuel, a professor and retired department chairman at the University of Missouri-Rolla.
Manuel claims that the interior of the sun is rich in iron and that the lighter hydrogen makes its way to the surface, making it seem that the sun is predominantly hydrogen. Typically, abundance numbers such as I quoted above are obtained from the spectra of the light emitted from the surface of a star. This "iron sun" hypothesis is something Manuel has been espousing for 40 years and flies in the face of the conventional wisdom that the sun is almost entirely hydrogen and helium.
Even more startling to me is Manuel''s assertion that our solar system, including the sun, did not form from a swirling cloud of nondescript gases and dust - the commonly accepted theory. Rather, Manuel thinks the solar system arose from the explosion of a single supernova, with the sun forming around the supernova''s collapsed core. His postulate is that the outer planets were formed from the outer envelopes of the debris of the exploding star, while the earth and other inner planets were formed from what was the inner regions of the iron-rich exploding star. This, he says, would account for the fact that the compositions of the planets are so different. The outer ones like Jupiter and Neptune are gaseous planets while Earth, Venus and Mars are rocky planets rich in iron and other heavy elements.
I get the impression that Manuel has had a hard time selling this hypothesis. However, I did note that a NASA or Jet Propulsion Lab Web site has a sketch of the sun that shows an iron core. Getting back to Christlieb and his colleagues, if Manuel is correct, it would seem that the newly found star would have even less iron compared to that in the sun, making their find even more impressive. Or does their star have an iron core too? If so, would the total iron content be more or less than 200,000 times less than the sun? Or is Manuel''s postulate totally wrong? If I find out the answers I''ll let you know.
If you search "iron sun" on the Web, you can see a really neat picture of the sun taken in the UV light emitted by ionized iron. The picture, which in essence shows the distribution of iron on the surface of the sun, was taken in 1996 from the SOHO spacecraft. If you don''t like the (false) green color I found on the University College London Web site, you can get it in blue, judging from the title of another Web site. Whatever your color choice, the picture shows that there''s an awful lot of whipping around and swirling of that iron on the sun''s surface.
Allen F. Bortrum
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