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Planetary nebula

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The image's organization is similar to that of a cat's eye. A bright almost pinpoint white circle in the center depicts the central star. The central star is encapsulated by a purple and red irregularly edged, elliptically shaped area that suggests a three dimensional shell. This is surrounded by a pair of superimposed circular regions of red with yellow and green edges, suggesting another three dimensional shell.
X-ray/optical composite image of the Cat's Eye Nebula

A planetary nebula is an emission nebula consisting of an expanding glowing shell of ionized gas and plasma ejected during the asymptotic giant branch phase of certain types of stars late in their life. The name originated with their first discovery in the 18th century because of their similarity in appearance to giant planets when viewed through small optical telescopes, and is otherwise unrelated to the planets of the solar system. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.

At the end of the star's life, during the red giant phase, the outer layers of the star are expelled via pulsations and strong stellar winds. Without these opaque layers, the remaining core of the star shines brightly and is very hot. The ultraviolet radiation emitted by this core ionizes the ejected outer layers of the star which radiate as a planetary nebula.

Star field with circular shell with green center and red at the edge of the shell.
NGC 2438

Planetary nebulae are important objects in astronomy because they play a crucial role in the chemical evolution of the galaxy, returning material to the interstellar medium which has been enriched in heavy elements and other products of nucleosynthesis (such as carbon, nitrogen, oxygen and calcium). In other galaxies, planetary nebulae may be the only objects observable enough to yield useful information about chemical abundances.

In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About a fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may all play a role.

Observations

Green roughly elliptical haze against a background of stars with red highlights especially at the outer edge of the shell.
NGC 6853, The Dumbbell Nebula
Credit: Robert J. Vanderbei

Planetary nebulae are generally faint objects, and none is visible to the naked eye. The first planetary nebula discovered was the Dumbbell Nebula in the constellation of Vulpecula, observed by Charles Messier in 1764 and listed as M27 in his catalogue of nebulous objects. To early observers with low-resolution telescopes, M27 and subsequently discovered planetary nebulae somewhat resembled the giant planets like Uranus, and William Herschel, discoverer of this planet, eventually coined the term 'planetary nebula' for them, although, as we now know, they are very different from planets.

Colorful shell which has an almost eye like appearance. The center shows the small central star with a blue circular area that could represent the iris. This is surrounded by an iris like area of concentric orange bands. This is surrounded by an eyelid shaped red area before the edge where plain space is shown. Background stars dot the whole image.
NGC 7293, The Helix Nebula
Credit: NASA, ESA, and C.R. O'Dell (Vanderbilt University)

The nature of planetary nebulae was unknown until the first spectroscopic observations were made in the mid-19th century. William Huggins was one of the earliest astronomers to study the optical spectra of astronomical objects, using a prism to disperse their light. On August 29, 1864, Huggins was the first to take the spectrum of a planetary nebula when he analyzed NGC 6543. His observations of stars showed that their spectra consisted of a continuum with many dark lines superimposed on them, and he later found that many nebulous objects such as the Andromeda Nebula (as it was then known) had spectra which were quite similar to this—these nebulae were later shown to be galaxies.

However, when he looked at the Cat's Eye Nebula, he found a very different spectrum. Rather than a strong continuum with absorption lines superimposed, the Cat's Eye Nebula and other similar objects showed only a small number of emission lines. The brightest of these was at a wavelength of 500.7 nanometres, which did not correspond with a line of any known element. At first it was hypothesized that the line might be due to an unknown element, which was named nebulium—a similar idea had led to the discovery of helium through analysis of the Sun's spectrum in 1868.

Spherical shell of colored area against background stars. Intricate cometary-like knots radiate inwards from the edge to about 1/3 of the way to the center. The center 1/2 contains brighter spherical shells that overlap each other and have rough edeges. Lone central star is visible in the middle. No background stars are visible.
NGC 2392, The Eskimo Nebula
Credit: NASA, ESA, Andrew Fruchter (STScI), and the ERO team (STScI + ST-ECF)

While helium was isolated on earth soon after its discovery in the spectrum of the sun, nebulium was not. In the early 20th century Henry Norris Russell proposed that rather than being a new element, the line at 500.7 nm was due to a familiar element in unfamiliar conditions.

Physicists showed in the 1920s that in gas at extremely low densities, electrons can populate excited metastable energy levels in atoms and ions which at higher densities are rapidly de-excited by collisions. Electron transitions from these levels in nitrogen and oxygen ions (O or OIII, O and N) give rise to the 500.7 nm line and other lines. These spectral lines, which can only be seen in very low density gases, are called forbidden lines. Spectroscopic observations thus showed that nebulae were made of extremely rarefied gas.

The central stars of planetary nebulae are very hot. Only once a star has exhausted all its nuclear fuel can it collapse to such a small size, and so planetary nebulae came to be understood as a final stage of stellar evolution. Spectroscopic observations show that all planetary nebulae are expanding. This led to the idea that planetary nebulae were caused by a star's outer layers being thrown into space at the end of its life.

Towards the end of the 20th century, technological improvements helped to further the study of planetary nebulae. Space telescopes allowed astronomers to study light emitted beyond the visible spectrum which is not detectable from ground-based observatories (because only radio waves and visible light penetrate the Earth's atmosphere). Infrared and ultraviolet studies of planetary nebulae allowed much more accurate determinations of nebular temperatures, densities and abundances. Charge-coupled device technology allowed much fainter spectral lines to be measured accurately than had previously been possible. The Hubble Space Telescope also showed that while many nebulae appear to have simple and regular structures from the ground, the very high optical resolution achievable by a telescope above the Earth's atmosphere reveals extremely complex morphologies.

Under the Morgan-Keenan spectral classification scheme, planetary nebulae are classified as Type-P, although this notation is seldom used in practice.

Origins

Central star has elongated S shaped curve of white emanating in opposite directions to the edge. A butterfly-like area surrounds the S shape with the S shape corresponding to the body of the butterfly.
Computer simulation of the formation of a planetary nebula from a star with a warped disk, showing the complexity which can result from a small initial asymmetry.
Credit: Vincent Icke

Stars weighing more than 8 solar masses (M⊙) will likely end their lives in a dramatic supernova explosion. Planetary nebula may result from the death of medium and low mass stars down to 0.8 M⊙.

Stars spend most of their lifetime shining as a result of nuclear fusion reactions that convert hydrogen to helium in the star's core. Outward pressure from fusion in the core balances inward collapse due to the star's own gravity. Such stars are said to be in the main sequence.

Medium to low mass stars run out of hydrogen in their cores after tens of millions to billions of years in the main sequence. Gravity compresses the core and it heats up. Currently the sun's core has a temperature of approximately 15 million K, but when it runs out of hydrogen, the compression of the core will cause the temperature to rise to about 100 million K.

The outer layers of the star expand enormously and become much cooler in response to the very high temperature of the core. The star becomes a red giant. The core continues to contract and heat up, and when its temperature reaches 100 million K, helium nuclei begin to fuse into carbon and oxygen. The resumption of fusion reactions stops the core's contraction. Helium burning soon forms an inert core of carbon and oxygen, with both a helium-burning shell and a hydrogen-burning shell surrounding it. In this last stage the star will observationally be a red giant again and structurally an asymptotic giant branch star.

Helium fusion reactions are extremely temperature sensitive, with reaction rates being proportional to T (under relatively low temperatures). This means that just a 2% rise in temperature more than doubles the reaction rate. The star becomes very unstable—a small rise in temperature leads to a rapid rise in reaction rates, which releases a lot of energy, increasing the temperature further. The helium-burning layer rapidly expands and therefore cools, which reduces the reaction rate again. Huge pulsations build up, which eventually become large enough to throw off the whole stellar atmosphere into space.

The ejected gases form a cloud of material around the now-exposed core of the star. As more and more of the atmosphere moves away from the star, deeper and deeper layers at higher and higher temperatures are exposed. When the exposed surface reaches a temperature of about 30,000 K, there are enough ultraviolet photons being emitted to ionize the ejected atmosphere, making it glow. The cloud has then become a planetary nebula.

Lifetime

After the asymptotic giant branch (AGB) phase, the short planetary nebula phase of stellar evolution begins as gases drift away from the central star at speeds of a few kilometers per second. The central star is the remnant of its AGB progenitor, an electron-degenerate carbon-oxygen core that has lost most of its hydrogen envelope due to mass loss on the AGB. As the gases expand, the central star undergoes a two stage evolution, first growing hotter as it continues to contract and hydrogen fusion reactions occur in the shell around the core and then slowly cooling once the hydrogen shell is exhausted through fusion and mass loss. In the second phase, it radiates away its energy and fusion reactions cease, as the central star is not heavy enough to generate the core temperatures required for carbon and oxygen to fuse. During the first phase the central star maintains constant luminosity while, at the same time, it grows ever hotter, eventually reaching temperatures around 100,000K. In the second phase, it eventually cools down so much that it doesn't give off enough ultraviolet radiation to ionize the increasingly distant gas cloud. The star becomes a white dwarf, and the gas cloud recombines, becoming invisible, ending the planetary nebula phase of evolution. For a typical planetary nebula, about 10,000 years passes between its formation and recombination of the star.

Galactic recyclers

Planetary nebulae play a very important role in galactic evolution. The early universe consisted almost entirely of hydrogen and helium, but stars create heavier elements via nuclear fusion. The gases of planetary nebulae thus contain a large proportion of elements such as carbon, nitrogen and oxygen, and as they expand and merge into the interstellar medium, they enrich it with these heavy elements, collectively known as metals by astronomers.

Subsequent generations of stars which form will then have a higher initial content of heavier elements. Even though the heavy elements will still be a very small component of the star, they have a marked effect on its evolution. Stars which formed very early in the universe and contain small quantities of heavy elements are known as Population II stars, while younger stars with higher heavy element content are known as Population I stars (see stellar population).

Characteristics

Physical characteristics

Elliptical shell with fine red outer edge surrounding region of yellow and then pink around a nearly circular blue area with the central star at its center. A few background stars are visible.
NGC 6720, The Ring Nebula
Credit: STScI/AURA

A typical planetary nebula is roughly one light year across, and consists of extremely rarefied gas, with a density generally from 100 to 10,000 particles per cm. (The Earth's atmosphere, by comparison, contains 2.5×10 particles per cm.) Young planetary nebulae have the highest densities, sometimes as high as 10 particles per cm. As nebulae age, their expansion causes their density to decrease. The masses of planetary range from 0.1 to 1 solar masses.

Radiation from the central star heats the gases to temperatures of about 10,000 K. The gas temperature in central regions is usually much high than at the periphery reaching 16,000–25,000 K. The volume in the vicinity of the central star is often filled with a very hot (coronal) gas having the temperature of about 1,000,000 K. This gas originates from the surface of the central star in the form of the fast stellar wind.

Nebulae may be described as matter bounded or radiation bounded. In the former case, there is not enough matter in the nebula to absorb all the UV photons emitted by the star, and the visible nebula is fully ionized. In the latter case, there are not enough UV photons being emitted by the central star to ionize all the surrounding gas, and an ionization front propagates outward into the circumstellar neutral envelope.

Numbers and distribution

About 3000 planetary nebulae are now known to exist in our galaxy, out of 200 billion stars. Their very short lifetime compared to total stellar lifetime accounts for their rarity. They are found mostly near the plane of the Milky Way, with the greatest concentration near the galactic center.

Morphology

Only about 20% of planetary nebulae are spherically symmetric (for example, see Abell 39). A wide variety of shapes exist with some very complex forms seen. Planetary nebulae are classified by different authors into: stellar, disk, ring, irregular, helical, bipolar, quadrupolar, and other types. Although the majority of them belong to just three types: spherical, elliptical and bipolar. The nebulae of the last type show the strongest concentration to the galactic plane and their progenitors are therefore relatively young massive stars. On the other hand spherical nebulae are likely produced by the old stars similar to the Sun.

The huge variety of the shapes is partially the projection effect—the same nebula when viewed under different angles will look differently. Nevertheless the reason for the huge variety of physical shapes is not fully understood, but may be caused the gravitational interactions with companion stars if the central stars are double stars. Another possibility is that planets disrupt the flow of material away from the star as the nebula forms. It has been determined that the more massive stars produces more irregularly shaped nebulae. In January 2005, astronomers announced the first detection of magnetic fields around the central stars of two planetary nebulae, and hypothesised that the fields might be partly or wholly responsible for their remarkable shapes.

Membership in clusters

Planetary nebulae have been detected as members in four globular clusters: Messier 15, Messier 22, NGC 6441 and Palomar 6. However, there has yet to be an established case of a planetary nebula discovered in an open cluster as based on a consistent set of distances, reddenings, and radial velocities. The cases of NGC 2348 in Messier 46, and NGC 2818 in the respective open cluster that is designated by the same name, are often cited as bona fide instances, however, they are instead line-of-sight coincidences granted the radial velocities between the clusters and planetary nebulae are discrepant.

Partly because of their small total mass, open clusters have relatively poor gravitational cohesion. Consequently, open clusters tend to disperse after a relatively short time, typically from 100 to 600 million years, because of external gravitational influences amid other factors. Under exceptional conditions, open clusters can remain intact for up to one billion years or more.

Theoretical models predict that planetary nebulae can form from main-sequence stars of between eight and one solar masses, which puts their age at 40 million years and older. Although there are a few hundred known open clusters within that age range, a variety of reasons limit the chances of finding a member of an open cluster in a planetary nebula phase. One such reason is that the planetary nebula phase for more massive stars belonging to younger clusters is on the order of thousands of years—a blink of the eye in cosmic terms.

Current issues in planetary nebula studies

A long standing problem in the study of planetary nebulae is that in most cases, their distances are very poorly determined. For a very few nearby planetary nebulae, it is possible to determine distances by measuring their expansion parallax high resolution observations taken several years apart will show the expansion of the nebula perpendicular to the line of sight, while spectroscopic observations of the Doppler shift will reveal the velocity of expansion in the line of sight. Comparing the angular expansion with the derived velocity of expansion will reveal the distance to the nebula.

The issue of how such a diverse range of nebular shapes can be produced is a controversial topic. Broadly, it is believed that interactions between material moving away from the star at different speeds gives rise to most shapes observed. However, some astronomers believe that double central stars must be responsible for at least the more complex and extreme planetary nebulae. One recent study has found that several planetary nebulae contain strong magnetic fields, something which has been hypothesized by Grigor Gurzadyan already in the 1960s. Magnetic interactions with ionized gas could be responsible for shaping at least some planetary nebulae.

There are two different ways of determining metal abundances in nebulae, which rely on different types of spectral lines—recombination lines and collisionally excited lines, and large discrepancies are sometimes seen between the results derived from the two methods. Some astronomers put this down to the presence of small temperature fluctuations within planetary nebulae; others claim that the discrepancies are too large to be explained by temperature effects, and hypothesize the existence of cold knots containing very little hydrogen to explain the observations. However, no such knots have yet been observed.

See also

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Subsequent evolutionary stage:

Template:Multicol-break General topics:

Otherwise related:

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References

  1. ^ Frankowski & Soker 2009, pp. 654–8
  2. ^ Kwok 2005, pp. 271–8
  3. Hubblesite.org 1997
  4. ^ Kwok 2000, pp. 1–7
  5. ^ Moore 2007, pp. 279–80
  6. Huggins & Miller 1864, pp. 437–44
  7. Bowen 1927, pp. 295–7
  8. Gurzadyan 1997
  9. Hora et al. 2004, pp. 296–301
  10. Kwok et al. 2006, pp. 445–6
  11. ^ Reed et al. 1999, pp. 2430–41
  12. Aller & Hyung 2003, p. 15
  13. Krause 1961, p. 187
  14. ^ Maciel, Costa & Idiart 2009, pp. 127–37
  15. Harpaz 1994, pp. 55–80
  16. ^ Harpaz 1994, pp. 99–112
  17. Iliadis 2007, pp. 18, 439–42
  18. Renzini 1987, pp. 391–400
  19. Kwok 2000, pp. 199–207
  20. Marochnik, Shukurov & Yastrzhembsky 1996, pp. 6–10
  21. ^ Osterbrock & Ferland 2005, p. 10
  22. Gurzadyan 1997, p. 238
  23. Gurzadyan 1997, pp. 130–7
  24. ^ Osterbrock & Ferland 2005, pp. 261–2
  25. Osterbrock & Ferland 2005, p. 207
  26. Parker et al. 2006, pp. 79–94
  27. ^ Majaess, Turner & Lane 2007, pp. 1349–60
  28. Jacoby, Ferland & Korista 2001, pp. 272–86
  29. Kwok & Su 2005, pp. L49–52
  30. ^ Kwok 2000, pp. 89–96
  31. Morris 1990, pp. 526–30
  32. SpaceDaily Express 2005 harvnb error: no target: CITEREFSpaceDaily_Express2005 (help)
  33. ^ Jordan, Werner & O'Toole 2005, pp. 273–9
  34. Kiss et al. 2008, pp. 399–404
  35. Mermilliod et al. 2001, pp. 30–9
  36. Allison 2006, pp. 56–8
  37. Soker 2002, pp. 481–6
  38. Gurzadyan 1997, p. 424
  39. Liu et al. 2000, pp. 585–587

Cited sources

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