Planetary Nebulæ: death throes of sunlike stars
Planetary Nebulæ are some of the prettiest objects we can see in a night even in
a backyard telescope. They show us the endgame of life for a typical star and also
forecast the fate of our Sun and solar system. Finally they start gaining the
recognition they deserve as some of the most revealing and useful objects in the universe.
Glowing like a multi-faceted jewel, the planetary nebula IC 418
lies about 2,000 light-years from Earth in the constellation Lepus.
Despite the name, these objects have nothing in common with ''planets''.
They do however represent the likely final episode of solar type stars.
A star is born, lives, grows old and dies. Most of its lifetime a star
shines by burning hydrogen into helium in its centre. A star starts
to die when it has exhausted the nuclear fuel in its core.
Its longevity depends upon its mass: the heavier the star, the sooner it dies.
Massive stars die very violently in a bright explosion, called a supernova.
The vast majority of stars, like our sun or up to eight times heavier, die more gracefully, more slowly.
After exhausting its thermonuclear fuel supply in the core, the outer layers fall inward.
On their way in they ignite, causing the outer material to be flung outward in an expanding cloud of gas.
When only a bit of hydrogen is left over the core the whole shell will be ejected.
When the remnant stellar core has become hot enough, this nebula will glow from the radiation of this exposed
hot core. It is visible as a planetary nebula. The remnant core will emerge
through the expanding veil of ejected material as a white dwarf.
A white dwarf is very dense. It has half the mass of the Sun, but is only the size of the Earth.
The white dwarf will very slowly fade away and over several billions of years turn into a dark
and invisible briquette, floating lifeless in the vast graveyard of space. Continued expansion
of the nebula at an average velocity of 90,000 km/h, combined with the decreasing
radiation of the cooling white dwarf causes the brightness of the nebula to decrease rapidly.
After roughly 25,000 years from its first appearance, the nebula would disappear from view.
It eventually disperses into the interstellar medium, enriching it with carbon, nitrogen and oxygen,
that were produced in the stellar interior. This material can be recycled to
form other stars and planets, and eventually life. You are made of star stuff, we all are.
The atoms of some of the elements that comprise our bodies were created in the depth of the stars.
What we are is literally stuff of the cosmos - atoms that have been recycled
many times before they came together to make you.
Different ways in which dying stars eject their outer layers as highly structured nebulæ.
A montage of pre- and true planetary nebulæ made with the Hubble Space Telescope Credits: Bruce
Balick, Howard Bond, Raghvendra Sahai, their collaborators, and NASA.
From left to right: M2-9, NGC 6826, Hourglass Nebula, NGC 3918, Egg Nebula, Cat's Eye Nebula, Hubble
5, NGC 7009, Red Rectangle, NGC 7662.
Their beauty is matched by the mystery. The basic question is: how do these nebulæ shape themselves ?
A most intriguing challenge is to understand how stars transform their surrounding
large spherical mass-loss shells in a couple of thousand years into the variety of shapes
and sizes observed in planetary nebulæ. There are a number of theories currently being investigated.
No consensus about the dominant physical process responsible for the shaping of planetary nebulæ has
emerged so far, but there is agreement that the shaping occurs during or soon after
the star ejects the nebula and the object is on its way of becoming a planetary nebula.
The details of the rate of evolution and the strength of the stellar wind during this
transition phase are essential ingredients in understanding the shaping of the planetary nebulæ.
However, both are very poorly known, either theoretically or observationally. To remedy this
Dr Griet Van de Steene in collaboration with Dr Peter Wood from the Australian National University,
and Dr Peter van Hoof from the Canadian Institute of Theoretical Astrophysics are studying a sample
of IR-selected stars which are becoming planetary nebulæ.
Images and spectra provide us with information about what has happened during the star's life and how it dies.
The Ring Nebula (M57) - HST picture
The nebula is about a light-year in diameter and is located some
2.000 light-years from Earth in the direction of the constellation Lyra.
The colors are approximately true colors. The color image was assembled
from three black-and-white photos taken through different color filters
with the Hubble telescope's Wide Field Planetary Camera 2.
Blue isolates emission from very hot helium, which is located primarily close to the
hot central star. Green represents ionized oxygen, which is located farther
from the star. Red shows ionized nitrogen, which is radiated from the coolest
gas, located farthest from the star. The gradations of color illustrate how
the gas glows because it is bathed in ultraviolet radiation from the
remnant central star, whose surface temperature is a white-hot 216.000 degrees Fahrenheit (120.000 degrees Celcius)
A typical spectrum of a planetary nebula contains several emission lines. The properties
of a planetary nebula (stellar temperature and luminosity, and chemical composition of the nebula)
can be determined using the observed spectrum. The influence of the nebular structure
on the determination of the abundances remains an issue.
Spectrum of NGC 3242 obtained with the 1.52-m telescope and the Boller \&
Chivens spectrograph at La Silla Observatory of the European Southern Observatory by Griet Van de Steene.
Picture By Bruce Balick.
Dr Griet Van de Steene in collaboration with Dr Peter van Hoof worked on photo-ionization
modelling in order to determine the chemical composition of planetary nebulæ.
Planetary Nebulæ are observable in far away galaxies
The spectra of planetary nebulæ include several bright emission lines, which make
them detectable and recognisable over large distances, not only in the obscured regions close to the center
of our own galaxy, but even in external galaxies, such as the Andromeda galaxy, and as far away as the
Dr. George Jacoby from the National Optical Astronomical Observatories in the USA
and Dr. Griet Van de Steene have identified 95 new candidate planetary nebulæ close to the center of our Galaxy.
They have obtained follow-up spectra for ~65 of these to confirm all but a couple
as bona fide nebulæ. These observations of the Galactic center nebulæ will help define the motions of stars
in the central "bar" of our Galaxy, as well as flagging any nebulæ that originated in
the halo of our Galaxy but are presently passing near the Galactic nucleus; already, two very fast moving candidates
have been identified as possible halo visitors. Thus far, only ~12 of the new ~90 planetary nebulæ in the Galactic
center have been analyzed to derive their chemical compositions. The chemical compositions appear to be similar to those found
in the Andromeda galaxy by Jacoby and Ciardullo. In most of the remaining cases, it will not be possible to make
the measurements because the nebulæ are extremely faint, being extinguished by an enormous of dust between
the Galactic center and the Earth.
Thus, each nebula that can be studied is an important one. We are continuing our analysis of the existing spectra.
Planetary Nebulæ can be observed out to large distances from the core of galaxies. The measurement
of their velocities provides the only way to study the dynamics and the distribution of dark matter in the
halos of elliptical galaxies.
Planetary Nebulæ are used as candlesticks to measure distances to other galaxies and in
this way contribute to unravelling the fate of the Universe.
The chemical composition of a planetary nebula is determined by the chemical composition
in the cloud of gas from which the progenitor star was formed and by the modification of these abundances by the nuclear
reactions during the star's life. Hence planetary nebulæ contribute to determining the chemical evolution of galaxies.
MSSSO image of the Andromeda Galaxy (M31). At a distance of 2900
kly, this spiral galaxy is our nearest large neighbour within the Local
The image was obtained with the 16 inch telescope and Nikkor 400mm
f/4.5 lens at SSO by the Imaging Team.
There seem to be several times more halo planetary nebulæ in M31 than in our own Galaxy.
Jacoby and collaborators have accumulated velocities for over 800 nebulæ in the nearby Andromeda galaxy.
They have measured the chemical compositions of 15 planetary nebulæ in M31.
From these measurements, it is clear that the stars in M31 are derived from a complex history of chemical
enrichment because they span a very wide range of compositions, from 20 times lower than the Sun to just slightly higher than the Sun.