How Far Are the Stars? (part 3)

In my last post, I showed how Cepheid variables allow us measure distances to distant stars and even to other galaxies. However, there is a limit to how far we can measure using Cepheids.  To measure the distance to the farthest galaxies, it takes a standard candle much brighter than a Cepheid. It takes a supernova.

Measuring by Supernova

Tycho Brahe

In November 1572, Tycho Brahe noticed among the stars of Cassiopeia a bright object no one had seen or catalogued before.  From November 2-6, this ‘star’ which had been invisible but now outshone all other stars, rivaled Venus in brightness.  It then gradually faded from view, remaining visible to the naked eye until 1574.  In his published work, Brahe termed this object stella nova, or ‘new star’ in Latin.  From then on, astronomers called any star that suddenly brightened by many magnitudes a ‘nova.’

In the early 20th century, Walter Baade and Fritz Zwicky were studying novae that seemed much more energetic than most.  During a 1931 lecture, Zwicky coined the term ‘supernova’ for an event that releases as much energy at once as the sun does over 10 million years.  (As it turns out, Brahe had observed a supernova, not a mere nova).

White Dwarfs

We now know that novae and one type of supernova occur due to white dwarfs accreting matter onto their surfaces.  All stars roughly as massive as our sun end up as white dwarfs.  In a white dwarf, the nuclear fusion which normally powers the star and resists gravitational collapse has ceased.  Yet, the white dwarf fails to collapse completely because of its extreme density; a white dwarf has approximately the sun’s mass in approximately the Earth’s volume.  Thus, the matter is so dense that any further compression would force multiple electrons into the same quantum state–which is disallowed according to the Pauli exclusion principle.  The resulting resistance to further compression becomes a force known as electron degeneracy pressure.

Occasionally, a white dwarf gravitationally bound to another star gains mass from that star.  Every star has a Roche lobe, which is the region of space in which all orbiting material remains bound to the star.  If, during stellar evolution, the companion of a white dwarf expands beyond its Roche lobe, some of its material, having escaped its gravity, can fall onto the white dwarf.  On the white dwarf’s surface, in-falling material, mostly hydrogen and helium, can attain temperatures and pressures sufficient to start nuclear fusion.  The resulting fusion of hydrogen into helium and helium into carbon and oxygen releases so much energy that the white dwarf suddenly becomes up to 50,000 times more luminous. The white dwarf has gone nova.  As dramatic as a nova explosion is, however, the material ejected is typically only about 1/10,000 of the sun’s mass–much less than the mass of the white dwarf.  Therefore, a particular star can go nova on many different occasions.

The Crab Nebula is a pulsar wind nebula associated with the 1054 supernova,
recorded by both Chinese and Islamic Astronomers.

There is a limit as to how much mass electron degeneracy pressure can support.  A white dwarf must have a mass less than 1.38 solar masses (the Chandrasekhar limit) to remain stable.  If a white dwarf in the scenario described above accretes enough mass to surpass that limit, the entire star becomes unstable, resulting in a explosion called a type Ia supernova.  Unlike a nova, a supernova cannot recur because the star has been destroyed.

Supernova Types

‘Type I’ refers to scheme established by Rudolph Minkowski and Fritz Zwicky which classifies supernovae based on their spectra.  Spectra of type II supernovae indicate the presence of hydrogen.  These are supernovae in which a star much more massive than our sun collapses and explodes, skipping a white dwarf phase altogether.  Type Ib and Ic supernovae occur when very massive stars which have lost hydrogen explode.  They lack hydrogen in their spectra, which puts them in type I, but they are more similar to type II supernovae in how they form.  Type Ia supernovae, in which white dwarfs explode, are the most interesting for our purposes here.

Standard Candles

In every type Ia supernova, then, the same amount of mass (about 1.38 solar masses) is exploding.  As a result, each type Ia supernova has the same intrinsic brightness, or luminosity.  Recognizing this, Walter Baade proposed using them as standard candles back in 1938.  Further, such a supernova is brilliant, rivaling the brightness of an entire galaxy, and therefore visible over much longer distances than Cepheids.  For these two reasons, type Ia supernovae are excellent standard candles for measuring distances to galaxies containing them.  With type Ia supernovae, we can measure distances many hundreds of millions of parsecs away, as compared to only about 29 million parsecs for Cepheids.

Champagne Supernova

There are two caveats, however.  First, astronomers using the Mauna Kea Observatory in Hawaii in 2003 observed an atypical type Ia supernova, which they dubbed the ‘Champagne Supernova’ (nicknamed after the Oasis song of 1996).  Somehow, this white dwarf managed two solar masses before exploding (rather than 1.38).  Some suspect that an unusually fast rotation may have allowed the extra mass to accrete, but this is an area of ongoing research–a reminder that whenever we think we have something figured out, nature can surprise us.

Second, although measruing galaxies hundreds of millions of parsecs away is a great achievement, we estimate that the observable universe is 28 billion parsecs across.  There are still other tools we must use to measure even more distant wonders.

Can’t see the video? Check out this video on Supernovas by clicking here.

The Incredible Journey of the Monarchs – on PBS

She Was Completely Transparent With Me
Creative Commons License photo credit: Randy Son Of Robert

What do you know about monarch butterflies?

A universal favorite, most people know that these showy orange and black butterflies fly south every year to spend the winter in Mexico. Many of you may have raised their black, yellow, and white caterpillars on Mexican milkweed as a class project or in your backyard.

But why do the adult butterflies migrate, and how do they get there and back? Who are the people and cultures they encounter as they traverse the continent from north to south each year? How did we learn about their migration, and what does it tell us about the natural world?

Creative Commons License photo credit: tlindenbaum

To answer these questions, and to see some amazing footage of millions of butterflies in flight and at their overwintering grounds, be sure to watch NOVA’s long-awaited special, “The Incredible Journey of the Monarchs.” It airs on PBS tomorrow night (Tuesday, January 27) at 7 p.m.

Inspired by Sue Halpern’s book, “Four Wings and a Prayer,” the filmmaker followed the butterflies in hot air balloons and high tech gliders, interviewing researchers and ordinary citizens in Canada, the USA, and Mexico to tell the story of these unusual butterflies and the unique phenomenon of their migration.

You can catch a quick preview of the show, learn about filmmaker Nick de Pencier, or see a list of monarch links and books at the NOVA website.

According to our friends in the monarch-watching business (see this film is “the best program ever done on monarch butterflies.” Don’t miss it!

Again, it airs in Houston on PBS (Channel 8) on Tuesday, January 27 at 7 p.m.

Starting Off With a Big Bang – Naturally

Creative Commons License photo credit: Eurritimia

Well, if another blog must be added to the ever-expanding blogosphere (which might now be growing at a rate similar to that of the universe itself), it makes sense to begin at the beginning of all energy-the “cosmogenesis,” when all matter, time and energy as we know it came into existence, commonly known as the “Big Bang.”

Now, as you can quickly discern, I have just opened a universe-sized can of worms here, as this “explosive” topic can be a source of endless spirited discussion among scientists, philosophers, theologians, and countless casually interested people with an opinion of some kind, so pretty much everyone. But that is exactly the point, as this blog is not intended to be a font of irrefutable truths, but rather an informal forum for interesting opinions and a starting point for conversation.

In any case, the universe was born and all matter and energy came into existence.


Creative Commons License photo credit: Space Ritual

Some 8 to 10 billion years after the universe as we know it was set into motion, our own sun formed in the Milky Way galaxy, and has ever since then been supplying Earth with a steady stream of energy; from direct forms, such as the sun’s rays warming the atmosphere, to indirect forms such as photosynthesis, in which plants convert solar radiation into stored chemical energy. Photosynthesis, incidentally, is the ultimate source of the energy in all fossil fuels, so any licensed driver better know about it.

For an interactive look at the basics of photosynthesis, click over to this site, courtesy of the clever people at the PBS show Nova (As a bonus, the explanatory text uses the common measure rhyme scheme.)

Of course, for the best three-minute tour from the Big Bang to the stuff that eventually turned into overpriced gasoline for your Hummer, visit the 18-screen video wall at the entrance to the Wiess Energy Hall here at the Houston Museum of Natural Science.

Humans have been using energy as long as they have been human, starting with the conversion of the caloric content of food into work – a change of chemical energy into kinetic energy. For an excellent primer on all forms of energy, check out the following link to our very own U. S. Department of Energy. Although, designed for kids, it’s a great overview for anyone.

And so, let the blogging begin. Your energetic reactions, comments and suggestions are encouraged.