Star count

Last updated December 01, 2024

Star counts are census counts of stars ^[1] and the statistical and geometrical methods used to correct the corresponding data for bias.^{[ citation needed ]} The surveys are most often made of nearby stars in the Milky Way galaxy.^{[ citation needed ]}

Reasons for star counts

When performing star counts, astronomers consider many different categories that have been created to classify a few stars that have been well studied. One of the hopes of studying the results of star counts is to discover new categories. Different counts typically seek to categorize stars for only a few of the qualities listed below, and determine how common each considered quality is and how stars of that kind are distributed.

Temperature: In astronomy, temperature is usually shown using the letter codes O B A F G K M running from 'blue' (type O, actually bluish white) through white (type F) to 'red' (type M, actually ruddy orange). Types L and T are used for brown dwarfs, whose 'colors' are in the infrared.
Size: Size is usually designated by Roman numerals I (supergiants) through V (dwarfs).
Age: Stars are usually grouped into Population I (young) and Population II (old).
Location: In the Milky Way galaxy the groups are described as thin disk , thick disk, central bulge, and halo.
Multiplicity: Most stars are members of double star, or triple star, or even double-double star systems. Our own sun appears to be unusual for not having a companion star.

There are many finer subdivisions in all of the above categories.

Bias

There are many unavoidable problems in counting stars for the purpose of getting an accurate picture of the distribution of stars in space. The effects of our point of view in the galaxy, the obscuring clouds of gas and dust in the galaxy, and especially the extreme range of inherent brightness, create a biased view of stars.

Stars vary far more in intrinsic brightness than they do in distance.
Our line of sight through the Milky Way is interrupted by great clouds of gas and dust, which block our view of stars more than a few thousand light-years away.
The Sun is located in the disk of the Milky Way, in the northern edge of the thin disk and on the inner edge of a spiral arm called the Orion–Cygnus Arm. There is good reason to believe that stars in the galaxy's thin disk are different from thicker part of the disk, and from the bulge and the halo. Some stars are obviously more common in spiral arms than in the disk in between the arms.

Knowing that these effects create bias, astronomers analyzing star counts attempt to find how much bias each effect has caused and then compensate for it as well as they can.

Inherent luminosity complications

The greatest problem biasing star counts is the extreme differences in inherent brightness of different sizes.

Heavy, bright stars (both giants and blue dwarfs) are the most common stars listed in general star catalogs, even though on average they are rare in space. Small dim stars (red dwarfs) seem to be the most common stars in space, at least locally, but can only be seen with large telescopes, and then only when they are within a few tens of light-years from Earth.

For example, the blue supergiant ζ Puppis is 400 million times more luminous than the nearest star, a red dwarf named Proxima, or α Centauri C. Even though Proxima is only 4.2 light-years away from us, it is so dim that it cannot be seen with the naked eye (one of its companions, α Centauri A, is visible). ζ Puppis is one of the brightest of the visible blue supergiants. It is so bright that it appears to be a second magnitude star, even though ζ Puppis is 1,399 light-years away.

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<span class="mw-page-title-main">Blue giant</span> Hot, giant star of early spectral type

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<span class="mw-page-title-main">Blue supergiant</span> Hot, luminous star with a spectral type of A9 or earlier

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<span class="mw-page-title-main">Outline of astronomy</span> Overview of the scientific field of astronomy

The following outline is provided as an overview of and topical guide to astronomy:

RS Puppis is a Cepheid variable star around 6,000 ly away in the constellation of Puppis. It is one of the biggest and brightest known Cepheids in the Milky Way galaxy and has one of the longest periods for this class of star at 41.5 days.

<span class="mw-page-title-main">Hypergiant</span> Rare star with tremendous luminosity and high rates of mass loss by stellar winds

A hypergiant (luminosity class 0 or Ia⁺) is a very rare type of star that has an extremely high luminosity, mass, size and mass loss because of its extreme stellar winds. The term hypergiant is defined as luminosity class 0 (zero) in the MKK system. However, this is rarely seen in literature or in published spectral classifications, except for specific well-defined groups such as the yellow hypergiants, RSG (red supergiants), or blue B(e) supergiants with emission spectra. More commonly, hypergiants are classed as Ia-0 or Ia⁺, but red supergiants are rarely assigned these spectral classifications. Astronomers are interested in these stars because they relate to understanding stellar evolution, especially star formation, stability, and their expected demise as supernovae. Notable examples of hypergiants include the Pistol Star, a blue hypergiant located close to the Galactic Center and one of the most luminous stars known; Rho Cassiopeiae, a yellow hypergiant that is one of the brightest to the naked eye; and Mu Cephei (Herschel's "Garnet Star"), one of the largest and brightest stars known.

The following outline is provided as an overview of and topical guide to galaxies:

References

↑ "Star count". Merriam Webster . Retrieved 2024-11-30.
1 2 Kron, Richard G. (1984). Capaccioli, Massimo (ed.). "Star Counts". Astronomy with Schmidt-Type Telescopes. Dordrecht: Springer Netherlands: 315–324. doi:10.1007/978-94-009-6387-0_53. ISBN 978-94-009-6387-0.

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[1] "Star count". Merriam Webster . Retrieved 2024-11-30.

[:0-2] 1 2 Kron, Richard G. (1984). Capaccioli, Massimo (ed.). "Star Counts". Astronomy with Schmidt-Type Telescopes. Dordrecht: Springer Netherlands: 315–324. doi:10.1007/978-94-009-6387-0_53. ISBN 978-94-009-6387-0.

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