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100th Gemini Paper Reveals White Dwarf Progenitors are Prolific Mass Expellers

January 27, 2005

A long-standing problem in understanding the evolution of stars has been determining the nature of the stellar progenitors for white dwarf stars. In particular, astronomers want to know how a rather massive star (up to seven times the mass of the Sun) can lose enough mass to become a white dwarf. Key questions include: Which main-sequence stars eventually end their life as white dwarfs? How much mass do they lose in late evolutionary stages? What process allows this to occur?

White Dwarfs and the Evolution of Stars

Gemini Observatory

Gemini adaptive optics image of a planetary nebula (BD+303639). Planetary nebulae often form around stars which expel mass rapidly late in life as they evolve into white dwarfs. This image was obtained using the University of Hawaii's Hokupa'a adaptive optics system on Gemini North.

Observations and theory give strong evidence that all stars expel a large fraction of their mass throughout their lifetimes. The most intensive phase of this mass loss takes place during a star’s late evolutionary phase. When a star nears the end of its life, its central region contains less fuel for hydrogen burning and the core region contracts until the temperature gets high enough for the nuclear fusion of helium to begin. The structure of the star changes dramatically as hydrogen in the shell surrounding the core also begins burning. Depending on the star’s initial mass on the main sequence (where a star spends most of its hydrogen-burning lifetime), it then enters an unstable period where variations in its temperature, radius and luminosity occur. This can result in structural changes in the star, such as the loss of its external layers.

For stars more than about seven times the mass of the Sun, the ultimate effect of these instabilities is a spectacular supernova explosion. Stars less than about seven solar masses enter a short phase (a few thousand years) that includes successive episodes of mass loss. This eventually leaves behind a stripped stellar core of carbon and oxygen mixed with a degenerate gas of electrons that determine the structure of the remnant. What’s left is called a white dwarf, an important end product of stellar evolution.

White dwarfs have an average diameter of about 10,000 kilometers, about the size of the Earth. However, their final masses are about half that of the Sun, which makes their density about a million times that of most common solid elements found on Earth. The properties of these stellar corpses are fascinating because of the curious nature of the degenerate electrons that provide the pressure to support them. The compressed electrons behave like a solid because of their high conductivity and incompressibility, but they are truly what is known as a degenerate gas. This incompressible quality of white dwarfs has led some call them, “the largest diamonds in the universe.”

The white dwarf phase of a star can last for billions of years, and during this time the object does not generate energy by thermonuclear reactions. The energy that radiates is sustained simply by cooling, just as a hot piece of iron metal emits radiation as it cools.

Some answers can be found in the 100th published paper based upon Gemini data. A Canadian, U.S., and Australian team led by Ph. D. student Jason Singh Kalirai of the University of British Columbia selected 24 individual white dwarfs* in the field of the rich open star cluster NGC 2099 (M37). This initial identification was made from analysis of deep wide-field imaging using the Canada-France-Hawaii Telescope. By following up on these imaging observations with subsequent spectroscopy from the Gemini North telescope, the team members assembled the largest spectroscopic sample ever obtained of white dwarfs in an individual star cluster. From these data they were able to constrain the relationship between the initial mass of a parent star on the main sequence and the final mass of the resulting white dwarf.

* Three of the 24 identified stars turned out not to be white dwarfs
and all stars in the study are fainter than V = 22.4

The result of their study indicates that stars with initial masses between 2.8 and 3.4 that of the Sun will lose 70-75% of their masses through stellar evolution.

The spectra for this study were obtained by Kalirai et al. using the Gemini Multi-object Spectrograph on Gemini North (GMOS-N) and the Keck Low-Resolution Infrared Spectrograph (LRIS) on Keck I.

Gemini Observatory

Figure 1. Spectral line profiles of the hydrogen Balmer lines of 16 white dwarfs in the open star cluster NGC 2099 with model fits (in red) courtesy of  Pierre Bergeron. The first six objects (WD 1- WD 7) have the highest signal-to-noise ratio and were obtained with Gemini/GMOS-North. The remaining stars (Keck objects) have lower signal-to-noise but have bluer spectral coverage (hence the fitting of the higher order Balmer lines).

Detailed modeling of the spectral features (Figure 1) allowed the team to derive pressures, temperatures and masses of the white dwarfs and from this infer their individual cooling ages. (A white dwarf’s cooling age is the total time that the star has spent since traversing from the tip of the asymptotic giant branch (AGB) down to its present white dwarf luminosity.) The team also calculated the progenitor main-sequence lifetime (tMS), which is the lifetime of the star from the time it turns on hydrogen burning in its core to the time it evolves to the tip of the AGB. To do this, the age of the parent stellar cluster (tcluster) was determined by fitting the appropriate isochrones to the “normal” stars of the open cluster NGC 2099. The team determined an age for the cluster of 650 million years.

A star’s lifetime on the main sequence (tMS), is simply the difference between the parent cluster’s age (tcluster), and the white dwarf cooling age (tcooling), which can be expressed as:

tMS = tcluster-tcooling

Not surprisingly, cooling ages vary between the individual white dwarfs in this open cluster, with the more massive ones taking the longest and the least massive cooling over the shortest period of time. In the equation above, greater values for tcooling correspond to a shorter main-sequence lifetime, and therefore to a more massive progenitor (since massive stars evolve faster than lower-mass ones).

Gemini Observatory

Figure 2. Top - The white dwarf initial-final mass relationship is shown for the 18 white dwarfs spectroscopically fit in this work (circles) and all previous constraints (triangles). Also shown are several semi-empirical and theoretical relations discussed in the Kalirai et al. paper. Bottom - A closer look at those white dwarfs that form the tight sequence with initial mass between 2.8 - 3.4 solar masses.

Kalirai and the team constructed a plot relating white dwarf masses in NGC 2099 to infer masses for main sequence stars (Figure 2). In the process they not only doubled the number of data points on the initial-final mass plane (Figure 2 – top), they also found a tight correspondence between main-sequence stars with an initial mass of 2.8 – 3.4 solar masses and a resulting white dwarf mass of 0.7 – 0.9 solar masses (Figure 2 – bottom).

The paper “The Initial-Final Mass Relationship: Spectroscopy of White Dwarfs in NGC 2099 (M37)” by J. S. Kalirai, H. B. Richer, D. Reitzel, B. M. S. Hansen, R. M. Rich, G. G Fahlman, B. K. Gibson and T. von Hippel is the 100th Gemini paper published in major refereed journals. It appeared in The Astrophysical Journal, vol 618, pp. 123-128, 10 January 2005. Kalirai et al. also published a companion paper in the same issue reporting that the mean derived mass of their white dwarf sample is 0.8 solar masses, about 0.2 solar masses larger than for the mean seen among field white dwarfs. Surprisingly, all these white dwarfs are found to have hydrogen, none of them are helium rich.

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