Tau Ceti

Short description: Single yellow-hued star in the constellation Cetus

For the video game, see Software:Tau Ceti (video game).

Tau Ceti

Location of τ Ceti (circled)

Observation data
Equinox J2000.0]] (ICRS)
Constellation | Cetus
Pronunciation  | /ˌtaʊ ˈsiːtaɪ/
Right ascension |  01h 44m 04.083s[1]
Declination | −15° 56′ 14.93″[1]
Apparent magnitude (V) | 3.50±0.01[2]
Characteristics
Evolutionary stage | Main sequence[3]
Spectral type | G8V[4]
U−B color index | +0.21[5]
B−V color index | +0.72[5]
Astrometry
Radial velocity (Rv)| −16.68±0.05[6] km/s
Proper motion (μ)|  RA: −1721.728[1] mas/yr
Dec.: +854.963[1] mas/yr
Parallax (π)| 273.8097 ± 0.1701[1] mas
Distance| 11.912 ± 0.007 ly
(3.652 ± 0.002 pc)
Absolute magnitude (MV)| 5.69±0.01[2]
Absolute bolometric
magnitude (Mbol)| 5.52±0.02[2]
Details
Mass| 0.800±0.008[7] M☉
Radius| 0.793±0.004[7] R☉
Luminosity| 0.488±0.010[2] L☉
Luminosity (visual, LV)| 0.45[nb 1] L☉
Surface gravity (log g)| 4.48±0.05[7] cgs
Temperature| 5,320±40[7] K
Metallicity| 28±3% Sun
Metallicity [Fe/H]| −0.55±0.05[8] dex
Rotation| 46±4 d[7]
Rotational velocity (v sin i)| 0.1±0.1[7] km/s
Age| 8–10[9] Gyr
Other designations

τ Cet, 52 Cet, BD−16°295, FK5 59, GJ 71, HD 10700, HIP 8102, HR 509, SAO 147986, LFT 159, LHS 146, LTT 935[5]

Database references
SIMBAD| data
Exoplanet Archive| data
ARICNS| data

Tau Ceti is a single star in the constellation Cetus. Its name is a Bayer designation that is Latinized from τ Ceti, and abbreviated Tau Cet or τ Cet. Spectrally, this star is similar to the Sun, although it has only about 78% of the Sun's mass. At a distance of just under 12 light-years (3.7 parsecs) from the Solar System, it is a relatively nearby star and the closest solitary G-class star. The star appears stable, with little stellar variation, and is metal-deficient (low in elements other than hydrogen and helium) relative to the Sun.

It can be seen with the unaided eye with an apparent magnitude of 3.5.[2] As seen from Tau Ceti, the Sun would be in the northern hemisphere constellation Boötes with an apparent magnitude of about 2.6.[nb 2][10]

Observations have detected more than ten times as much dust surrounding Tau Ceti as is present in the Solar System. Tau Ceti has been an object of interest for exoplanet searches, and a number of candidate planets have been proposed,[11] but as of 2025[update] there remains no unambiguous evidence of planets.[12] Because of its debris disk, any planet orbiting Tau Ceti would face far more impact events than present day Earth. Despite this hurdle to habitability, its solar analog (Sun-like) characteristics have led to widespread interest in the star. Given its stability, similarity and relative proximity to the Sun, Tau Ceti is consistently listed as a target for the search for extraterrestrial intelligence (SETI).[13]

## Contents

* 1 Name
* 2 Motion
* 3 Physical properties
* 3.1 Rotation
* 3.2 Metallicity
* 3.3 Luminosity and variability
* 4 Search for planets
* 4.1 Planet candidates
* 4.2 Tau Ceti e
* 4.3 Tau Ceti f
* 4.4 Debris disk
* 4.5 Habitability
* 5 In fiction
* 6 See also
* 7 Notes
* 8 References
* 9 Further reading
* 10 External links

## Name

The name "Tau Ceti" is the Bayer designation for this star, established in 1603 as part of German celestial cartographer Johann Bayer's Uranometria star catalogue: it is "number T" in Bayer's sequence of constellation Cetus. In the catalogue of stars in the Calendarium of Al Achsasi al Mouakket, written at Cairo about 1650, this star was designated Thālith al Naʽāmāt (ثالث النعامات – thālith al-naʽāmāt), which was translated into Latin as Tertia Struthionum, meaning the third of the ostriches.Cite error: Closing `</ref>` missing for `<ref>` tag Consequently, the Chinese name for τ Ceti itself is "the Fifth Star of Square Celestial Granary" (Chinese: 天倉五; pinyin: Tiān Cāng wǔ).[14]

## Motion

The proper motion of a star is its angular rate of movement across the celestial sphere, determined by comparing its position relative to more distant background objects. Moving at 1.9 arcseconds per year (1900 years per degree),[nb 3] Tau Ceti is considered to be a high-proper-motion star. A high proper motion is an indicator of closeness to the Sun:[15] nearby stars can traverse an angle of arc across the sky more rapidly than the distant background stars and are thus good candidates for parallax studies. In the case of Tau Ceti, the parallax measurements indicate a distance of 11.9 ly. This makes it one of the closest star systems to the Sun and the next-closest spectral class-G star after Alpha Centauri A.[16]

The radial velocity of a star is the component of its motion that is toward or away from the Sun. It can be determined by measuring the star's spectrum: due to the Doppler shift, the absorption lines in the spectrum of a star will be shifted slightly toward the red (or longer wavelengths) if the star is moving away from the observer, or toward blue (or shorter wavelengths) when it moves toward the observer. In the case of Tau Ceti, the radial velocity is about −17 km/s, with the negative value indicating that it is moving toward the Sun.[17] The star will make its closest approach to the Sun in about 43,000 years, when it comes to within 10.6 ly (3.25 pc).[18]

The distance to Tau Ceti, along with its proper motion and radial velocity, together give the motion of the star through space. The space velocity relative to the Sun is 37.2 km/s.[19] This result can then be used to compute an orbital path of Tau Ceti through the Milky Way. It has a mean galacto-centric distance of 9.7 kiloparsecs (32000 ly) and an orbital eccentricity of 0.22.[20]

## Physical properties

The Sun (left) is both larger and somewhat hotter than the less active Tau Ceti (right).

The Tau Ceti system is believed to have only one stellar component. A dim optical companion has been observed with magnitude 13.1. As of 2000, it was 137 arcseconds distant from the primary. It may be gravitationally bound, but it is considered more likely to be a line-of-sight coincidence.[21][22][23]

Most of what is known about the physical properties of Tau Ceti and its system has been determined through spectroscopic measurements. By comparing the spectrum to computed models of stellar evolution, the age, mass, radius and luminosity of Tau Ceti can be estimated. However, using an astronomical interferometer, measurements of the radius of the star can be made directly to an accuracy of 0.5%.[2] Through such means, the radius of Tau Ceti has been measured to be 79.3%±0.4% of the solar radius.[2] This is about the size that is expected for a star with somewhat lower mass than the Sun.[24]

### Rotation

The rotation period for Tau Ceti was measured by periodic variations in the classic H and K absorption lines of singly ionized calcium (Ca II). These lines are closely associated with surface magnetic activity,[25] so the period of variation measures the time required for the activity sites to complete a full rotation about the star. By this means the rotation period for Tau Ceti is estimated to be 34 d.[3] Due to the Doppler effect, the rotation rate of a star affects the width of the absorption lines in the spectrum (light from the side of the star moving away from the observer will be shifted to a longer wavelength; light from the side moving towards the observer will be shifted toward a shorter wavelength). By analyzing the width of these lines, the rotational velocity of a star can be estimated. The projected rotation velocity for Tau Ceti is

veq · sin i ≈ 1 km/s,

where veq is the velocity at the equator, and i is the inclination angle of the rotation axis to the line of sight. For a typical G8 star, the rotation velocity is about 2.5 km/s. The relatively low rotational velocity measurements may indicate that Tau Ceti is being viewed from nearly the direction of its pole.[26][27]

More recently, a 2023 study has estimated a rotation period of 46±4 d and a veq sin i of 0.1±0.1 km/s, corresponding to a pole-on inclination of 7°±7°.[7]

### Metallicity

The chemical composition of a star provides important clues to its evolutionary history, including the age at which it formed. The interstellar medium of dust and gas from which stars form is primarily composed of hydrogen and helium with trace amounts of heavier elements. As nearby stars continually evolve and die, they seed the interstellar medium with an increasing portion of heavier elements. Thus younger stars tend to have a higher portion of heavy elements in their atmospheres than do the older stars. These heavy elements are termed "metals" by astronomers, and the portion of heavy elements is the metallicity.[28] The amount of metallicity in a star is given in terms of the ratio of iron (Fe), an easily observed heavy element, to hydrogen. A logarithm of the relative iron abundance is compared to the Sun. In the case of Tau Ceti, the atmospheric metallicity is

[FeH]≈−0.50 dex,

equivalent to about a third the solar abundance. Past measurements have varied from −0.13 to −0.60.[29][30]

This lower abundance of iron indicates that Tau Ceti is almost certainly older than the Sun. Its age had previously been estimated to be 5.8 Gyr, but is now thought to be around 9 Gyr.[9] This compares with 4.57 Gyr for the Sun. However, age estimates for Tau Ceti can range from 4.4 to 12 Gyr, depending on the model adopted.[24]

Besides rotation, another factor that can widen the absorption features in the spectrum of a star is pressure broadening. The presence of nearby particles affects the radiation emitted by an individual particle. So the line width is dependent on the surface pressure of the star, which in turn is determined by the temperature and surface gravity. This technique was used to determine the surface gravity of Tau Ceti. The log g, or logarithm of the star's surface gravity, is about 4.4, very close to the log g = 4.44 for the Sun.[29]

### Luminosity and variability

The luminosity of Tau Ceti is equal to only 55% of the Sun's luminosity.[20] A terrestrial planet would need to orbit this star at a distance of about 0.7 astronomical unit|AU to match the solar insolation level of Earth. This is approximately the same as the average distance between Venus and the Sun.

The chromosphere of Tau Ceti—the portion of a star's atmosphere just above the light-emitting photosphere—currently displays little or no magnetic activity, indicating a stable star.[31] One 9-year study of temperature, granulation, and the chromosphere showed no systematic variations; Ca II emissions around the H and K infrared bands show a possible 11-year cycle, but this is weak relative to the Sun.[26] Alternatively it has been suggested that the star could be in a low-activity state analogous to a Maunder Minimum—a historical period, associated with the Little Ice Age in Europe, when sunspots became exceedingly rare on the Sun's surface.[32][33] Spectral line profiles of Tau Ceti are extremely narrow, indicating low turbulence and observed rotation.[34] The star's asteroseismological oscillations have an amplitude about half that of the Sun and a lower mode lifetime.[2]

## Search for planets

The principal factors driving research interest in Tau Ceti are its proximity, its Sun-like characteristics, and the implications for possible life on its planets. For categorization purposes, Hall and Lockwood report that "the terms 'solarlike star', 'solar analog', and 'solar twin' [are] progressively restrictive descriptions".[35]

In 1988, radial-velocity observations ruled out any periodical variations attributable to massive planets around Tau Ceti inside of Jupiter-like distances.[36][37] Ever more precise measurements continue to rule out such planets, at least until December 2012.[37] The velocity precision reached is about 11 m/s measured over a 5-year time span.[38] This result excludes hot Jupiters and probably excludes any planets with minimal mass greater than or equal to Jupiter's mass and with orbital periods less than 15 years.[39] In addition, a survey of nearby stars by the Hubble Space Telescope's Wide Field and Planetary Camera was completed in 1999, including a search for faint companions to Tau Ceti; none were discovered to limits of the telescope's resolving power.[40]

However, these searches only excluded larger brown dwarf bodies and closer orbiting giant planets, so smaller, Earth-like planets in orbit around the star were not precluded.[40] If hot Jupiters were to exist in close orbit, they would likely disrupt the star's habitable zone; their exclusion was thus considered positive for the possibility of Earth-like planets.[36][41] General research has shown a positive correlation between the presence of planets and a relatively high-metallicity parent star, suggesting that stars with lower metallicity such as Tau Ceti have a lower chance of having planets.[42]

The Tau Ceti planetary system[11][43] Companion
(in order from star) | Mass | Semimajor axis
(AU) | Orbital period
(days) | Eccentricity | Inclination | Radius

|
|
|
|
|
|

g (unconfirmed) | ≥1.75+0.25
−0.40 M⊕ | 0.133+0.001
−0.002 | 20.00+0.02
−0.01 | 0.06 ± 0.13  | —  | —
h (unconfirmed) | ≥1.83+0.68
−0.26 M⊕ | 0.243 ± 0.003  | 49.41+0.08
−0.10 | 0.23+0.16
−0.15 | —  | —
e (dubious) | ≥3.93+0.83
−0.64 M⊕ | 0.538 ± 0.006  | 162.87+1.08
−0.46 | 0.18+0.18
−0.14 | —  | —
f (unconfirmed) | ≥3.93+1.05
−1.37 M⊕ | 1.334+0.017
−0.044 | 636.13+11.70
−47.69 | 0.16+0.07
−0.16 | —  | —
Debris disk | 6.2+9.8
−4.6–52+3
−8 AU | 35±10° | —

### Planet candidates

On December 19, 2012, evidence was presented that suggested a system of five candidate planets orbiting Tau Ceti.[8] The planets' estimated minimum masses were between 2 and 6 Earth masses, with orbital periods ranging from 14 to 640 days. One of them, Tau Ceti e, appeared to orbit about half as far from Tau Ceti as Earth does from the Sun. With Tau Ceti's luminosity of 52% that of the Sun and a distance from the star of 0.552 AU, the planet would receive 1.71 times as much stellar radiation as Earth does, slightly less than Venus with 1.91 times Earth's. Nevertheless, some research placed it within the star's habitable zone.[44][45] The Planetary Habitability Laboratory estimated that Tau Ceti f, which receives 28.5% as much starlight as Earth, would be within the star's habitable zone, albeit narrowly.[46]

New results were published in August 2017.[11] They confirmed Tau Ceti e and f as candidates but failed to consistently detect planets b (which may be a false negative), c (whose weakly defined apparent signal was correlated to stellar rotation), and d (which did not show up in all data sets). Instead, they found two new planetary candidates, g and h, with orbits of 20 and 49 days. The signals detected from the candidate planets have radial velocities as low as 30 cm/s, and the experimental method used in their detection, as it was applied to HARPS, could in theory have detected down to around 20 cm/s.[11] The updated 4-planet model is dynamically packed and potentially stable for billions of years.

In 2019, a paper published in Astronomy & Astrophysics suggested that Tau Ceti could have a Jupiter or super-Jupiter based on a tangential astrometric velocity of around 11.3 m/s. The exact size and position of this conjectured object have not been determined, though it is at most 5 Jupiter masses if it orbits between 3 and 20 AU.[47][nb 4] A 2020 Astronomical Journal study by astronomers Jamie Dietrich and Daniel Apai analyzed the orbital stability of the known planets, assuming the 2017 4-planet model, and, considering statistical patterns identified from hundreds of other planetary systems, explored the orbits in which the presence of additional, yet-undetected planets are most likely. This analysis predicted three additional planets at orbits coinciding with planet candidates b, c, and d.[49] The close match between the independently predicted planet periods and the periods of the three planet candidates previously identified in radial velocity data could support the genuine planetary nature of these candidates,[49] although they were rejected by the 2017 paper.[11] Furthermore, the study also predicted at least one yet-undetected planet between planets e and f, i.e., within the habitable zone.[49] This predicted exoplanet was identified as PxP-4.

All proposed planet candidates remain unconfirmed; studies of Tau Ceti's radial velocity in 2019, 2021 and 2025 were unable to confirm any planets.[50][51][12] In particular, a 2025 study using ESPRESSO data did not detect any planets, while being sensitive to 1.7 M⊕ planets with periods up to 100 days, and 2–5 M⊕ planets in the habitable zone. These results do not support the existence of Tau Ceti e, while planets g & h are close to the detection limit and planet f is below it.[12][nb 5] While weak evidence was found for a 20-day signal (corresponding to Tau Ceti g), it is not statistically significant and its planetary nature is considered doubtful.[12]

Since Tau Ceti is likely aligned in such a way that it is nearly pole-on to Earth (as indicated by its rotation),[7] if its planets share this alignment and have nearly face-on orbits, they would be less similar to Earth's mass and more to Neptune, Saturn, or Jupiter. For example, were Tau Ceti f's orbit inclined 70 degrees from being face-on to Earth, its mass would be 4.18+1.12
−1.46 Earth masses, making it a middle-to-low end super-Earth. However, these scenarios are not necessarily true; since Tau Ceti's debris disk has an inclination of 35±10, the planets' orbits could be similarly inclined. If the debris disk and f's orbits were assumed to be equal, f would be between 5.56+1.48
−1.94 and 9.30+2.48
−3.24 Earth masses, making it slightly more likely to be a mini-Neptune. On top of that, the lower the inclination of the planetary orbits the less stable they tend to be over a given time period, as the planets would have greater masses and therefore more gravitational pull which would in turn disturb the orbital stability of neighbouring planets. So, for example, if as estimated in Korolik et al 2023 Tau Ceti has a pole-on inclination of around 7 degrees, and the postulated planets do as well, then those planets' orbits would be verging on instability within just a 10 million year timeframe, and therefore it is extremely unlikely they would have survived for the billions of years that make up the lifetime of the star system.[7]

### Tau Ceti e

Main article: Astronomy:Tau Ceti e

Tau Ceti e is a candidate[11] planet orbiting Tau Ceti that was first proposed in 2012 by statistical analyses of the data of the star's variations in radial velocity that were obtained using HIRES, AAPS, and HARPS.[8][52] Its possible properties were refined in 2017:[11] if confirmed, it would orbit at a distance of 0.552 AU (between the orbits of Venus and Mercury in the Solar System) with an orbital period of 168 days and has a minimum mass of 3.93 Earth masses. If Tau Ceti e possessed an Earth-like atmosphere, the surface temperature would be around 68 °C (154 °F).[53] Based upon the incident flux upon the planet, a study by Güdel et al. (2014) speculated that the planet may lie outside the habitable zone and closer to a Venus-like world.[54] As of 2025[update], the existence of this planet is doubtful as attempts to detect it with the ESPRESSO spectrograph have failed, despite being sensitive to it.[12]

### Tau Ceti f

Main article: Astronomy:Tau Ceti f

Tau Ceti f is a candidate[11] planet orbiting Tau Ceti that was proposed in 2012 by statistical analyses of the star's variations in radial velocity, and also recovered by further analysis in 2017.[8] It is of interest because its orbit places it in Tau Ceti's extended habitable zone.[55] However, a 2015 study implies that it would have been in the temperate zone for less than one billion years, so there may not be a detectable biosignature.[56][57][58]

Few properties of the planet are known other than its orbit and mass. It orbits Tau Ceti at a distance of 1.35 AU (near Mars's orbit in the Solar System) with an orbital period of 642 days and has a minimum mass of 3.93 Earth masses.[11]

However, a reanalysis of the data in 2021 provided an in-depth study of the HARPS spectrograph systematics, showing that the 600-day signal was likely a spurious combination of instrumental systematics with a potential 1000-day yet unknown signal.[51]

### Debris disk

In 2004, a team of UK astronomers led by Jane Greaves discovered that Tau Ceti has more than ten times the amount of cometary and asteroidal material orbiting it than does the Sun. This was determined by measuring the disk of cold dust orbiting the star produced by collisions between such small bodies.[59] This result puts a damper on the possibility of complex life in the system, because any planets would suffer from large impact events roughly ten times more frequently than present day Earth. Greaves noted at the time of her research that "it is likely that [any planets] will experience constant bombardment from asteroids of the kind believed to have wiped out the dinosaurs".[60] Such bombardments would inhibit the development of biodiversity between impacts.[61]

The debris disk was discovered by measuring the amount of radiation emitted by the system in the far infrared portion of the spectrum. The disk forms a symmetric feature that is centered on the star, and its outer radius averages 55 AU. The lack of infrared radiation from the warmer parts of the disk near Tau Ceti implies an inner cut-off at a radius of 10 AU. By comparison, the Solar System's Kuiper belt extends from 30 to 50 AU. To be maintained over a long period of time, this ring of dust must be constantly replenished through collisions by larger bodies.[59] The bulk of the disk appears to be orbiting Tau Ceti at a distance of 35–50 AU, well outside the orbit of the habitable zone. At this distance, the dust belt may be analogous to the Kuiper belt that lies outside the orbit of Neptune in the Solar System.[59]

Tau Ceti shows that stars need not lose large disks as they age, and such a thick belt may not be uncommon among Sun-like stars.[62] Tau Ceti's belt is only 1/20 as dense as the belt around its young neighbor, Epsilon Eridani.[59] The relative lack of debris around the Sun may be the unusual case: one research-team member suggests the Sun may have passed close to another star early in its history and had most of its comets and asteroids stripped away.[60] Stars with large debris disks have changed the way astronomers think about planet formation because debris disk stars, where dust is continually generated by collisions, appear to form planets readily.[62]

### Habitability

Tau Ceti's habitable zone—the locations where liquid water could be present on an Earth-sized planet—spans a radius of 0.55–1.16 AU, where 1 AU is the average distance from the Earth to the Sun.[63] Primitive life on Tau Ceti's planet candidates may reveal itself through an analysis of atmospheric composition via spectroscopy, if the composition is unlikely to be abiotic, just as oxygen on Earth is indicative of life.[64]

Tau Ceti could have been a search target for the canceled Terrestrial Planet Finder

The most optimistic search project to date was Project Ozma, which was intended to "search for extraterrestrial intelligence" (SETI) by examining selected stars for indications of artificial radio signals. It was run by the astronomer Frank Drake, who selected Tau Ceti and Epsilon Eridani as the initial targets. Both are located near the Solar System and are physically similar to the Sun. No artificial signals were found despite 200 hours of observations.[65] Subsequent radio searches of this star system have turned up negative.

This lack of results has not dampened interest in observing the Tau Ceti system for biosignatures. In 2002, astronomers Margaret Turnbull and Jill Tarter developed the Catalog of Nearby Habitable Systems (HabCat) under the auspices of Project Phoenix, another SETI endeavour. The list contained more than 17000 theoretically habitable systems, approximately 10% of the original sample.[66] The next year, Turnbull would further refine the list to the 30 most promising systems out of 5000 within 100 light-years from the Sun, including Tau Ceti; this will form part of the basis of radio searches with the Allen Telescope Array.[67] She chose Tau Ceti for a final shortlist of just five stars suitable for searches by the (now cancelled)[68] Terrestrial Planet Finder telescope system, commenting that "these are places I'd want to live if God were to put our planet around another star".[69]

## In fiction

This section is an excerpt from Stars in fiction#Real stars[ edit ]

Tau Ceti is also the setting of Andy Weir's 2021 novel, Project Hail Mary, and its 2026 film adaptation of the same name.[70]

## See also

* List of potentially habitable exoplanets
* List of nearest terrestrial exoplanet candidates
* List of nearest G-type stars

## Notes

1. ↑ From knowing the absolute visual magnitude of Tau Ceti, MV∗=5.69, and the absolute visual magnitude of the Sun, MV⊙=4.83, the visual luminosity of Tau Ceti can therefore be calculated: LV∗/LV⊙=100.4(MV⊙−MV∗).
2. ↑ From Tau Ceti the Sun would appear on the diametrically opposite side of the sky at the coordinates RA = 13h 44m 04s, Dec = 15° 56′ 14″, which is located near Tau Boötis. The absolute magnitude of the Sun is 4.8, so, at a distance of 3.65 pc, the Sun would have an apparent magnitude m=Mv+5⋅(log103.64−1)=2.6.
3. ↑ The net proper motion is given by μ=μδ2+μα2⋅cos2δ=1907.79mas/y, where μα and μδ are the components of proper motion in the RA and declination respectively, and δ is the declination. See: Majewski, Steven R. (2006). "Stellar Motions". University of Virginia. http://www.astro.virginia.edu/class/majewski/astr551/lectures/VELOCITIES/velocities.html.
4. ↑ If a planet is confirmed to be the cause of this signal, as of August 2020 it would be designated as Tau Ceti i in accordance with IAU exoplanet naming policies.[48]
5. ↑ Based on their original published masses,[8] these results also rule out the existence of planets b, c & d, which were already rejected in 2017.[11]

## References

1. ↑ 1.0 1.1 1.2 1.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 Teixeira, T. C.; Kjeldsen, H.; Bedding, T. R.; Bouchy, F.; Christensen-Dalsgaard, J.; Cunha, M. S.; Dall, T. et al. (January 2009). "Solar-like oscillations in the G8 V star τ Ceti". Astronomy and Astrophysics 494 (1): 237–242. doi:10.1051/0004-6361:200810746. Bibcode: 2009A&A...494..237T.
3. ↑ 3.0 3.1 Baliunas, S.; Sokoloff, D.; Soon, W. (1996). "Magnetic Field and Rotation in Lower Main-Sequence Stars: an Empirical Time-dependent Magnetic Bode's Relation?". Astrophysical Journal Letters 457 (2): L99. doi:10.1086/309891. Bibcode: 1996ApJ...457L..99B.
4. ↑ Keenan, Philip C; McNeil, Raymond C (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series 71: 245. doi:10.1086/191373. Bibcode: 1989ApJS...71..245K.
5. ↑ 5.0 5.1 5.2 "Tau Cet". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Tau+Cet.
6. ↑ Nidever, David L. et al. (2002). "Radial Velocities for 889 Late-Type Stars". The Astrophysical Journal Supplement Series 141 (2): 503–522. doi:10.1086/340570. Bibcode: 2002ApJS..141..503N.
7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 7.7 7.8 Korolik, Maria; Roettenbacher, Rachael M.; Fischer, Debra A. et al. (September 1, 2023). "Refining the Stellar Parameters of τ Ceti: a Pole-on Solar Analog". The Astronomical Journal 166 (3): 123. doi:10.3847/1538-3881/ace906. ISSN 0004-6256. Bibcode: 2023AJ....166..123K.
8. ↑ 8.0 8.1 8.2 8.3 8.4 Tuomi, M.; Jones, H. R. A.; Jenkins, J. S.; Tinney, C. G.; Butler, R. P.; Vogt, S. S.; Barnes, J. R.; Wittenmyer, R. A. et al. (2013). "Signals embedded in the radial velocity noise". Astronomy & Astrophysics 551: A79. doi:10.1051/0004-6361/201220509. Bibcode: 2012yCat..35510079T.
9. ↑ 9.0 9.1 Tang, Y. K.; Gai, N. (February 2011). "Asteroseismic modelling of the metal-poor star τ Ceti". Astronomy & Astrophysics 526: A35. doi:10.1051/0004-6361/201014886. Bibcode: 2011A&A...526A..35T.
10. ↑ Cox, Arthur N., ed. (2001-04-20), Allen's Astrophysical Quantities (Fourth ed.), Springer, p. 382, ISBN 0-387-95189-X.
11. ↑ 11.00 11.01 11.02 11.03 11.04 11.05 11.06 11.07 11.08 11.09 Feng, Fabo et al. (2017). "Color Difference Makes a Difference: Four Planet Candidates around Tau Ceti". The Astronomical Journal 154 (4): 135. doi:10.3847/1538-3881/aa83b4. Bibcode: 2017AJ....154..135F.
12. ↑ 12.0 12.1 12.2 12.3 12.4 Figueira, P.; Faria, J. P.; Silva, A. M.; Castro-González, A.; Silva, J. Gomes da; Sousa, S. G.; Bossini, D.; Zapatero-Osorio, M. R. et al. (July 10, 2025). "A comprehensive study on radial velocity signals using ESPRESSO: Pushing precision to the 10 cm/s level". Astronomy and Astrophysics 700: A174. doi:10.1051/0004-6361/202553869. Bibcode: 2025A&A...700A.174F.
13. ↑ Rutkowski, Chris A. (2010), The Big Book of UFOs, Dundurn, p. 33, ISBN 978-1554887606, https://books.google.com/books?id=cqmizCB7iacC&pg=PA33
14. ↑ 陳輝樺, ed (July 10, 2006). "Error: no `|title=` specified when using {{Cite web}}" (in zh). http://aeea.nmns.edu.tw/2006/0607/ap060710.html.Error:+no+`|title=`+specified when+using+{{[[Template:Cite+web|Cite+web]]}}&rft.atitle=&rft.date=July+10,+2006&rft_id=http://aeea.nmns.edu.tw/2006/0607/ap060710.html&rfr_id=info:sid/en.wikibooks.org:Astronomy:Tau_Ceti">
15. ↑ Reid, Neill (February 23, 2002). "Meeting the neighbours: NStars and 2MASS". Space Telescope Science Institute. http://www-int.stsci.edu/~inr/nstars2.html.
16. ↑ Henry, Todd J. (October 1, 2006). "The One Hundred Nearest Star Systems". Research Consortium on Nearby Stars. http://www.chara.gsu.edu/RECONS/TOP100.htm.
17. ↑ Butler, R. P.; Marcy, G. W.; Williams, E.; McCarthy, C.; Dosanjh, P.; Vogt, S. S. (1996). "Attaining Doppler Precision of 3 M s-1". Publications of the Astronomical Society of the Pacific 108: 500. doi:10.1086/133755. Bibcode: 1996PASP..108..500B.
18. ↑ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics 575: 13, doi:10.1051/0004-6361/201425221, A35, Bibcode: 2015A&A...575A..35B. (Data for Tau Ceti is in the CDS)
19. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
20. ↑ 20.0 20.1 Porto de Mello, G. F.; del Peloso, E. F.; Ghezzi, L. (2006). "Astrobiologically interesting stars within 10 parsecs of the Sun". Astrobiology 6 (2): 308–331. doi:10.1089/ast.2006.6.308. PMID 16689649. Bibcode: 2006AsBio...6..308P.
21. ↑ Kaler, James. "Tau Ceti". University of Illinois. http://stars.astro.illinois.edu/sow/taucet.html.
22. ↑ "00-06 hour section". United States Naval Observatory. http://ad.usno.navy.mil/wds/Webtextfiles/wdsnewframe1.html.
23. ↑ Pijpers, F. P.; Teixeira, T. C.; Garcia, P. J.; Cunha, M. S.; Monteiro, M. J. P. F. G. (2003). "Interferometry and asteroseismology: The radius of τ Ceti". Astronomy & Astrophysics 401 (1): L15–L18. doi:10.1051/0004-6361:20030837. Bibcode: 2003A&A...406L..15P.
24. ↑ 24.0 24.1 Di Folco, E.; Thévenin, F.; Kervella, P.; Domiciano de Souza, A.; du Foresto; V. Coudé; Ségransan, D. et al. (2004). "VLTI near-IR interferometric observations of Vega-Like Stars". Astronomy and Astrophysics 426 (2): 601–617. doi:10.1051/0004-6361:20047189. Bibcode: 2004A&A...426..601D.
25. ↑ "H-K Project: Overview of Chromospheric Activity". Mount Wilson Observatory. http://www.mtwilson.edu/hk/Overview/.
26. ↑ 26.0 26.1 Gray, D. F.; Baliunas, S. L. (1994). "The activity cycle of tau Ceti". Astrophysical Journal 427 (2): 1042–1047. doi:10.1086/174210. Bibcode: 1994ApJ...427.1042G.
27. ↑ Hall, J. C.; Lockwood, G. W.; Gibb, E. L. (1995). "Activity cycles in cool stars. 1: Observation and analysis methods and case studies of four well-observed examples". Astrophysical Journal 442 (2): 778–793. doi:10.1086/175483. Bibcode: 1995ApJ...442..778H.
28. ↑ Carraro, G.; Ng, Y. K.; Portinari, L. (1999). "Age Metallicity Relation and Star Formation History of the Galactic Disk". Monthly Notices of the Royal Astronomical Society 296 (4): 1045–1056. doi:10.1046/j.1365-8711.1998.01460.x. Bibcode: 1998MNRAS.296.1045C.
29. ↑ 29.0 29.1 de Strobel; G. Cayrel; Hauck, B.; François, P.; Thevenin, F.; Friel, E.; Mermilliod, M. et al. (1991). "A catalogue of Fe/H determinations". Astronomy and Astrophysics Supplement Series 95 (2): 273–336. Bibcode: 1992A&AS...95..273C.
30. ↑ Flynn, C.; Morell, O. (1997). "Metallicities and kinematics of G and K dwarfs". Monthly Notices of the Royal Astronomical Society 286 (3): 617–625. doi:10.1093/mnras/286.3.617. Bibcode: 1997MNRAS.286..617F.
31. ↑ Frick, P.; Baliunas, S. L.; Galyagin, D.; Sokoloff, D.; Soon, W. (1997). "Wavelet Analysis of Stellar Chromospheric Activity Variations". The Astrophysical Journal 483 (1): 426–434. doi:10.1086/304206. Bibcode: 1997ApJ...483..426F.
32. ↑ Judge, P. G.; Saar, S. H. (July 18, 1995). "The outer solar atmosphere during the Maunder Minimum: A stellar perspective". The Astrophysical Journal (High Altitude Observatory) 663 (1): 643–656. doi:10.1086/513004. Bibcode: 2007ApJ...663..643J.
33. ↑ Judge, Philip G.; Saar, Steven H.; Carlsson, Mats; Ayres, Thomas R. (2004). "A Comparison of the Outer Atmosphere of the "Flat Activity" Star τ Ceti (G8 V) with the Sun (G2 V) and α Centauri A (G2 V)". The Astrophysical Journal 609 (1): 392–406. doi:10.1086/421044. Bibcode: 2004ApJ...609..392J.
34. ↑ Smith, G.; Drake, J. J. (July 1987). "The wings of the calcium infrared triplet lines in solar-type stars". Astronomy and Astrophysics 181 (1): 103–111. Bibcode: 1987A&A...181..103S.
35. ↑ Hall, J. C.; Lockwood, G. W. (2004). "The Chromospheric Activity and Variability of Cycling and Flat Activity Solar-Analog Stars". The Astrophysical Journal 614 (2): 942–946. doi:10.1086/423926. Bibcode: 2004ApJ...614..942H.
36. ↑ 36.0 36.1 Campbell, Bruce; Walker, G. A. H. (August 1988). "A Search for Substellar Companions to Solar-Type Stars". Astrophysical Journal 331: 902–921. doi:10.1086/166608. Bibcode: 1988ApJ...331..902C.
37. ↑ 37.0 37.1 "Tables of Stars monitored by spectroscopy, with NO planet found". Extrasolar Planets Encyclopaedia. http://exoplanet.eu/list_no.html. Retrieved 2007-09-28.
38. ↑ Endl, M.; Kurster, M.; Els, S. (2002). "The planet search program at the ESO Coud´e Echelle spectrometer". Astronomy & Astrophysics 392 (2): 585–594. doi:10.1051/0004-6361:20020937. Bibcode: 2002A&A...392..671E.
39. ↑ Walker, Gordon A. H. et al. (1995). "A Search for Jupiter-Mass Companions to Nearby Stars". Icarus 116 (2): 359–375. doi:10.1006/icar.1995.1130. Bibcode: 1995Icar..116..359W. However, this does not exclude the possibility of a large planet with a mass greater than Jupiter's and an orbital plane that is nearly perpendicular to the line of sight.
40. ↑ 40.0 40.1 Schroeder, D. J. et al. (2000). "A Search for Faint Companions to Nearby Stars Using the Wide Field Planetary Camera 2". Astronomical Journal 119 (2): 906–922. doi:10.1086/301227. Bibcode: 2000AJ....119..906S.
41. ↑ "Tau Ceti". Sol Company. http://www.solstation.com/stars/tau-ceti.htm.
42. ↑ Gonzalez, G. (March 17–21, 1997). "The Stellar Metallicity – Planet Connection". Brown Dwarfs and Extrasolar Planets (ASP Conference Series) 134: 431. Bibcode: 1998ASPC..134..431G.
43. ↑ MacGregor, Meredith A et al. (2016). "ALMA Observations of the Debris Disk of Solar Analogue Tau Ceti". The Astrophysical Journal 828 (2): 113. doi:10.3847/0004-637X/828/2/113. Bibcode: 2016ApJ...828..113M.
44. ↑ "Tau Ceti's planets nearest around single, Sun-like star". BBC News. December 19, 2012. https://www.bbc.co.uk/news/science-environment-20770103.
45. ↑ "Tau Ceti May Have a Habitable Planet". Astrobiology Magazine. December 19, 2012. http://www.astrobio.net/pressrelease/5220/tau-ceti-may-have-a-habitable-planet.
46. ↑ Torres, Abel Mendez (December 28, 2012). "Two Nearby Habitable Worlds?". Planetary Habitability Laboratory. University of Puerto Rico. http://phl.upr.edu/press-releases/twonearbyhabitableworlds.
47. ↑ Kervella, Pierre; Arenou, Frédéric et al. (2019). "Stellar and substellar companions of nearby stars from Gaia DR2". Astronomy & Astrophysics 623: A72. doi:10.1051/0004-6361/201834371. ISSN 0004-6361. Bibcode: 2019A&A...623A..72K. ""We also detect the signature of a possible planet of a few Jovian masses orbiting τ Ceti…The observed signal could be explained for example, by a Jupiter analog orbiting at 5au."".
48. ↑ "Naming of Exoplanets". IAU. https://www.iau.org/public/themes/naming_exoplanets/.
49. ↑ 49.0 49.1 49.2 Dietrich, Jamie; Apai, Dániel (October 27, 2020). "An Integrated Analysis with Predictions on the Architecture of the tau Ceti Planetary System, Including a Habitable Zone Planet". The Astronomical Journal 161 (1): 17. doi:10.3847/1538-3881/abc560. Bibcode: 2021AJ....161...17D.
50. ↑ Coffinet, A. et al. (September 2019). "New wavelength calibration of the HARPS spectrograph". Astronomy & Astrophysics 629: A27. doi:10.1051/0004-6361/201833272. Bibcode: 2019A&A...629A..27C.
51. ↑ 51.0 51.1 Cretignier, Michael et al. (September 2021). "YARARA: Significant improvement in RV precision through post-processing of spectral time series". Astronomy & Astrophysics 653: A43. doi:10.1051/0004-6361/202140986. Bibcode: 2021A&A...653A..43C.
52. ↑ "Four Exoplanets Detected around Nearby Star Tau Ceti | Astronomy". http://www.sci-news.com/astronomy/tau-ceti-exoplanets-05117.html.
53. ↑ Giovanni F. Bignami (2015). The Mystery of the Seven Spheres: How Homo sapiens will Conquer Space. Springer. ISBN 9783319170046. , Page 110.
54. ↑ Güdel, M.; Dvorak, R.; Erkaev, N.; Kasting, J.; Khodachenko, M.; Lammer, H.; Pilat-Lohinger, E.; Rauer, H. et al. (2014). "Protostars and Planets VI". in Beuther, Henrik; Klessen, Ralf S.; Dullemond, Cornelis P. et al.. Tucson: University of Arizona Press. pp. 883–906. doi:10.2458/azu_uapress_9780816531240-ch038. ISBN 978-0-8165-3124-0. Bibcode: 2014prpl.conf..883G.
55. ↑ "Two Nearby Habitable Worlds?". Planetary Habitability Laboratory @ UPR Arecibo. http://phl.upr.edu/press-releases/twonearbyhabitableworlds.
56. ↑ Wall, Mike (April 24, 2015). "Nearby Alien Planets Not So Life-Friendly After All". https://www.space.com/29191-exoplanets-tau-ceti-alien-life.html.
57. ↑ Arizona State University. "Tau Ceti: The next Earth? Probably not" (in en). https://phys.org/news/2015-04-tau-ceti-earth.html.
58. ↑ Pagano, Michael et al. (April 2015), "The Chemical Composition of τ Ceti and Possible Effects on Terrestrial Planets", The Astrophysical Journal 803 (2): 90, doi:10.1088/0004-637X/803/2/90, 90, Bibcode: 2015ApJ...803...90P.
59. ↑ 59.0 59.1 59.2 59.3 Greaves, J. S.; Wyatt, M. C.; Holland, W. S.; Dent, W. R. F. (2004). "The debris disc around tau Ceti: a massive analogue to the Kuiper Belt". Monthly Notices of the Royal Astronomical Society 351 (3): L54–L58. doi:10.1111/j.1365-2966.2004.07957.x. Bibcode: 2004MNRAS.351L..54G.
60. ↑ 60.0 60.1 McKee, Maggie (July 7, 2004). "Life unlikely in asteroid-ridden star system". New Scientist. http://media.newscientist.com/article.ns?id=dn6123.
61. ↑ Schirber, Michael (March 12, 2009). "Cometary Life Limit". NASA Astrobiology. http://www.astrobio.net/news/modules.php?op=modload&name=News&file=article&sid=3066&mode=thread&order=0&thold=0.
62. ↑ 62.0 62.1 Greaves, Jane S. (January 2005). "Disks Around Stars and the Growth of Planetary Systems". Science 307 (5706): 68–71. doi:10.1126/science.1101979. PMID 15637266. Bibcode: 2005Sci...307...68G.
63. ↑ Cantrell, Justin R et al. (October 2013). "The Solar Neighborhood XXIX: The Habitable Real Estate of Our Nearest Stellar Neighbors". The Astronomical Journal 146 (4): 99. doi:10.1088/0004-6256/146/4/99. Bibcode: 2013AJ....146...99C.
64. ↑ Woolf, Neville; Angel, J. Roger (September 1998). "Astronomical Searches for Earth-like Planets and Signs of Life". Annual Review of Astronomy and Astrophysics 36 (1): 507–537. doi:10.1146/annurev.astro.36.1.507. Bibcode: 1998ARA&A..36..507W.
65. ↑ Alexander, Amir (2006). "The Search for Extraterrestrial Intelligence, A Short History". The Planetary Society. http://www.planetary.org/explore/topics/seti/seti_history_05.html.
66. ↑ Turnbull, Margaret C. (March 2003). "Target Selection for SETI. I. A Catalog of Nearby Habitable Stellar Systems". Astrophysical Journal Supplement Series 145 (1): 181–198. doi:10.1086/345779. Bibcode: 2003ApJS..145..181T.
67. ↑ "Stars and Habitable Planets". Sol Company. http://www.solstation.com/habitable.htm.
68. ↑ "NASA budget statement". Planetary Society. 2006-02-06. http://www.planetary.org/about/press/releases/2006/0206_Planetary_Society_Charges.html.
69. ↑ "Astronomer Margaret Turnbull: A Short-List of Possible Life-Supporting Stars". American Association for the Advancement of Science. February 18, 2006. http://www.aaas.org/news/releases/2006/0218habitable.shtml.
70. ↑ Monica Young (19 March 2026). "Explore the Worlds of Project Hail Mary". Sky and Telescope. https://skyandtelescope.org/astronomy-news/explore-the-worlds-of-project-hail-mary/.

## Further reading

* Pagano, Michael et al. (April 2015), "The Chemical Composition of τ Ceti and Possible Effects on Terrestrial Planets", The Astrophysical Journal 803 (2): 90, doi:10.1088/0004-637X/803/2/90, 90, Bibcode: 2015ApJ...803...90P.
* Lawler, S. M. et al. (2014). "The debris disc of solar analogue τ Ceti: Herschel observations and dynamical simulations of the proposed multiplanet system". Monthly Notices of the Royal Astronomical Society 444 (3): 2665. doi:10.1093/mnras/stu1641. Bibcode: 2014MNRAS.444.2665L. https://pure.uva.nl/ws/files/2141414/158265_The_debris_disc.pdf. Retrieved 2018-11-04.
* Teixeira, T. C. et al. (January 2009), "Solar-like oscillations in the G8 V star τ Ceti", Astronomy and Astrophysics 494 (1): 237–242, doi:10.1051/0004-6361:200810746, Bibcode: 2009A&A...494..237T.
* di Folco, E. et al. (November 2007), "A near-infrared interferometric survey of debris disk stars. I. Probing the hot dust content around ɛ Eridani and τ Ceti with CHARA/FLUOR", Astronomy and Astrophysics 475 (1): 243–250, doi:10.1051/0004-6361:20077625, Bibcode: 2007A&A...475..243D.
* Rammacher, W.; Cuntz, M. (September 2003), "Acoustic Heating Models for the Basal Flux Star τ Ceti Including Time-dependent Ionization: Results for Ca II and Mg II Emission", The Astrophysical Journal 594 (1): L51–L54, doi:10.1086/378312, Bibcode: 2003ApJ...594L..51R.
* Gray, David F.; Baliunas, Sallie L. (June 1994), "The Activity Cycle of tau Ceti", Astrophysical Journal 427: 1042, doi:10.1086/174210, Bibcode: 1994ApJ...427.1042G.
* Arribas, S.; Martinez-Roger, C. (1988), Cayrel de Strobel, G.; Spite, Monique, eds., "Iron Lines and Surface Gravity Determination for τ Ceti", The Impact of Very High S/N Spectroscopy on Stellar Physics: Proceedings of the 132nd Symposium of the International Astronomical Union held in Paris, France, June 29-July 3, 1987. International Astronomical Union. Symposium no. 132 (Dordrecht: Kluwer Academic Publishers) 132: p. 445, Bibcode: 1988IAUS..132..445A.

## External links

* Tau Ceti at Jim Kaler's STARS site
* Tau Ceti: Life Amidst Catastrophe? at Centauri Dreams

Template:Tau Ceti

* v
* t
* e

← Celestial objects within 5–10 light-years →

| Primary member type|

Celestial objects by systems. Secondary members are listed in small print.

| Main-sequence
stars|

| A-type|

* Sirius (α CMa) (8.60±0.04 ly)
* white dwarf B

|

M-type
(red dwarfs)|

* Barnard's Star (5.980±0.003 ly)
* planet b
* Wolf 359 (7.856±0.031 ly)
* Lalande 21185 (8.307±0.014 ly)
* L 726-8 (8.73±0.06 ly)
* red dwarf UV Cet
* Ross 154 (9.60±0.05 ly)

| Brown dwarfs|

| L-type|

* Luhman 16 (6.59±0.06 ly)
* T-type brown dwarf B

|

| Sub-brown dwarfs
and rogue planets|

| Y-type|

* WISE 0855−0714 (7.27±0.13 ly)

|

Italic are systems without known trigonometric parallax.

* v
* t
* e

Cetus constellation

Stars
(list)|

| Bayer|

* α (Menkar)
* β (Diphda)
* γ (Kaffaljidhma)
* δ
* ε
* ζ (Baten Kaitos)
* η
* θ
* ι
* κ1
* κ2
* λ
* μ
* ν
* ξ1
* ξ2
* ο (Mira)
* π
* ρ
* σ
* τ
* υ
* φ1
* φ2
* φ3
* φ4
* χ

|

Flamsteed|

* 1
* 2
* 3
* 6
* 7
* 9
* 10
* 11
* 12
* 13
* 14
* 15
* 18
* 20
* 21
* 25
* 26
* 27
* 28
* 29
* 30
* 32
* 33
* 34
* 35
* 36
* 37
* 38
* 39
* 40
* 41
* 42
* 43
* 44
* 46
* 47
* 48
* 49
* 50
* 56
* 57
* 58
* 60
* 61
* 62
* 63
* 64
* 66
* 67
* 69
* 70
* 71
* 75
* 77
* 79
* 80
* 81
* 84
* 93
* 94
* 95
* 25 Ari

Variable|

* T
* RR
* TV
* TW
* UU
* VZ (Mira B)
* WW
* WX
* XY
* XZ
* YZ
* ZZ
* AA
* AB
* AD
* AR
* BG
* BK
* CF
* DK
* EH
* EL
* EO
* ES

HR|

* 9
* 10
* 12
* 16
* 31
* 37
* 51
* 61
* 66
* 72
* 108
* 115
* 118
* 150
* 159
* 172
* 173
* 174
* 190
* 197
* 201
* 206
* 210
* 218
* 220
* 227
* 228
* 232
* 247
* 251
* 263
* 320
* 325
* 387
* 388
* 392
* 394
* 404
* 405
* 406
* 416
* 425
* 448
* 466
* 473
* 492
* 500
* 507
* 513
* 560
* 608
* 611
* 616
* 625
* 638
* 651
* 672
* 684
* 692
* 693
* 697
* 713
* 719
* 725
* 732
* 735
* 737
* 745
* 751
* 766
* 770
* 775
* 783
* 784
* 795
* 796
* 816
* 870
* 908
* 926
* 942
* 9054
* 9095
* 9096
* 9101

HD|

* 1690
* 1879
* 2268
* 2638
* 4747
* 5319
* 6037
* 6718
* 7449
* 8713
* 8896
* 9690
* 9731
* 10024
* 10725
* 11365
* 11396
* 11506
* 11964
* 12116
* 12702
* 13004
* 13546
* 13763
* 15115
* 16008
* 16031
* 17001
* 224349
* 224693 (Axólotl)

Gliese|

* Gliese 40
* Gliese 105
* GJ 1002
* GJ 1005
* GJ 1057
* GJ 2012

Other|

* BD−17 63
* Cayrel's Star
* CFBDS J005910.90–011401.3
* CS 31082-001
* DENIS-P J020529.0−115925
* GD 40
* HIP 5158
* HIP 11952
* L 870-2
* LHS 1140
* Luyten 726-8 (UV/BL)
* NGC 156
* NGC 302
* NGC 308
* NGC 310
* PSR B0031−07
* PSR J0034−0534
* PSR J0108−1431
* SDSS J001820.5−093939.2
* SDSS J0106−1000
* ULAS J003402.77−005206.7
* WD J2356-209
* WASP-26
* WASP-44
* WASP-71
* WISE J0254+0223

Nebulae|

| Planetary|

* BoBn 1
* NGC 246

|

Galaxies|

| Messier|

* 77

|

NGC|

* 17
* 35
* 45
* 47
* 50
* 54
* 59
* 61
* 62
* 64
* 65
* 66
* 73
* 77
* 102
* 107
* 113
* 114
* 117
* 118
* 120
* 124
* 132
* 135
* 142
* 143
* 144
* 145
* 151
* 154
* 155
* 157
* 161
* 163
* 165
* 166
* 167
* 168
* 170
* 171
* 172
* 173
* 177
* 178
* 179
* 187
* 191
* 192
* 195
* 196
* 197
* 201
* 207
* 209
* 210
* 216
* 217
* 219
* 223
* 227
* 230
* 232
* 235A
* 235B
* 237
* 239
* 244
* 245
* 247
* 255
* 259
* 263
* 268
* 270
* 271
* 273
* 274
* 275
* 276
* 277
* 279
* 283
* 284
* 285
* 286
* 291
* 293
* 297
* 298
* 301
* 303
* 307
* 309
* 320
* 321
* 325
* 327
* 329
* 331
* 333
* 333B
* 335
* 336
* 337
* 337A
* 340
* 341
* 341B
* 342
* 343
* 344
* 345
* 347
* 349
* 350
* 351
* 352
* 353
* 355
* 356
* 357
* 359
* 363
* 364
* 367
* 369
* 377
* 391
* 413
* 417
* 426
* 428
* 429
* 430
* 435
* 442
* 445
* 448
* 450
* 478
* 480
* 481
* 487
* 493
* 497
* 519
* 521
* 530
* 533
* 535
* 538
* 539
* 540
* 541
* 543
* 545
* 547
* 548
* 550
* 554A
* 554B
* 555
* 556
* 557
* 558
* 560
* 564
* 565
* 567
* 570
* 577
* 578
* 583
* 584
* 585
* 586
* 589
* 593
* 594
* 596
* 599
* 600
* 601
* 615
* 617
* 622
* 624
* 635
* 636
* 640
* 647
* 648
* 649
* 655
* 667
* 681
* 682
* 690
* 699
* 701
* 702
* 707
* 713
* 715
* 720
* 725
* 726
* 731
* 734
* 747
* 748
* 755
* 756
* 758
* 762
* 767
* 768
* 773
* 779
* 787
* 788
* 790
* 799
* 800
* 806
* 808
* 809
* 811
* 814
* 815
* 825
* 827
* 829
* 830
* 831
* 833
* 835
* 836
* 837
* 838
* 839
* 840
* 842
* 844
* 848
* 849
* 850
* 851
* 853
* 858
* 859
* 863
* 864
* 867
* 868
* 872
* 873
* 874
* 878
* 879
* 880
* 881
* 883
* 887
* 892
* 894
* 895
* 899
* 902
* 905
* 907
* 908
* 921
* 926
* 929
* 934
* 936
* 941
* 942
* 943
* 944
* 945
* 947
* 948
* 950
* 951
* 955
* 958
* 960
* 963
* 965
* 966
* 967
* 975
* 977
* 981
* 985
* 988
* 989
* 991
* 993
* 997
* 998
* 1004
* 1007
* 1008
* 1009
* 1010
* 1011
* 1013
* 1015
* 1016
* 1017
* 1018
* 1019
* 1020
* 1021
* 1022
* 1026
* 1032
* 1033
* 1034
* 1035
* 1038
* 1041
* 1042
* 1043
* 1044
* 1045
* 1046
* 1047
* 1048
* 1048A
* 1051
* 1052
* 1055
* 1063
* 1064
* 1065
* 1069
* 1070
* 1071
* 1072
* 1073
* 1074
* 1075
* 1076
* 1078
* 1080
* 1085
* 1087
* 1090
* 1094
* 1095
* 1101
* 1104
* 1105
* 1107
* 1128
* 1137
* 1141
* 1142
* 1149
* 1153
* 1194
* 1211
* 1218
* 1219
* 1254
* 1280
* 7807
* 7808
* 7813
* 7821
* 7828
* 7829

Other|

* Arp 147
* Arp 256
* 3C 15
* 3C 17
* 3C 75
* Cetus Dwarf Spheroidal galaxy
* HCM-6A
* Holmberg 15A
* IC 1613
* IRAS F01475-0740
* Markarian 573
* Markarian 1014
* Markarian 1018
* Markarian 1044
* NAB 0205+024
* PHL 938
* PKS 0048-097
* PKS 0106+013
* PKS 0119-046
* PKS 0139-097
* PKS 0215+015
* PKS 0237-233
* PKS 0306+102
* QSO B0137+012
* QSO B0302-003
* SDSS J0303-0019
* SMM J02399-0136
* SXDF-NB1006-2
* 9Spitch
* Ton S180
* UM 673
* VV 114
* Wolf–Lundmark–Melotte

Galaxy
clusters|

* Abell 85
* Abell 119
* Abell 133
* Abell 151
* Abell 168
* Abell 194
* Abell 209
* Abell 222
* Abell 223
* Abell 267
* Abell 370
* Abell 400
* HCG 16
* IRC 0218
* JKCS 041
* RX J0152.7-1357

Other|

* GRB 000911
* GRB 041006
* GRB 050908
* GRB 060908
* GRB 091127
* SN 1984L
* SN 2005gj
* SN 2005hk

* v
* t
* e

2012 in space

* « 2011

2013 »

Space probe
launches|

* Van Allen Probes

Comets|

* C/2011 Q2 (McNaught)
* C/2012 C2 (Bruenjes)
* C/2006 S3 (LONEOS)
* C/2013 L2 (Catalina)
* C/2010 R1 (LINEAR)
* C/2011 U3 (PANSTARRS)
* C/2011 UF305 (LINEAR)
* C/2011 R1 (McNaught)
* C/2013 F1 (Boattini)
* C/2013 G2 (McNaught)
* C/2012 J1 (Catalina)

NEOs|

* Asteroid close approaches
* 2012 EG5
* 2012 TV
* 2012 TC4
* 2012 KP24
* 2012 BX34
* 2012 FP35
* 2012 KT42

Exoplanets|

* Gliese 667 Cc
* Alpha Centauri Bb
* Gliese 163 c
* HD 40307 e
* HD 40307 f
* HD 40307 g
* Kappa Andromedae b
* KELT-2Ab
* Kepler-23b
* Kepler-32b
* Kepler-32c
* Kepler-34b
* Kepler-36b
* Kepler-42c
* Kepler-47b
* Kepler-47c
* Kepler-56
* Kepler-80
* Kepler-88
* Kepler-89
* PH1b
* Tau Ceti e
* Tau Ceti f

Space
exploration|

* ANUSAT
* Curiosity
* Dragon C2+
* Edoardo Amaldi ATV
* Ekspress AM4
* Explorer 8
* Fobos-Grunt
* Kedr
* Kosmos 2176
* Kosmos 2261
* Kounotori 3
* Navid
* PharmaSat
* Progress M-13M
* Progress M-14M
* Progress M-15M
* Sfera
* Shenzhou 9
* Solar Anomalous and Magnetospheric Particle Explorer
* Soyuz TMA-03M
* Soyuz TMA-04M
* Soyuz TMA-05M
* Soyuz TMA-22
* SpaceX CRS-1
* TacSat-3
* USA-226
* Yinghuo-1

* Category:2011 in space — Category:2012 in space — Category:2013 in space

* v
* t
* e

2017 in space

* « 2016

2018 »

Impact events|

* Bolides in 2017
* 2017 China bolide

Selected NEOs|

* Asteroid close approaches
* 2012 TC4
* 2013 SY99 (announced)
* 2017 AG13
* 2014 JO25
* 2016 WF9
* 2017 BQ6
* 2017 BS5
* 2017 SX17
* 3122 Florence
* C/2015 ER61 (PANSTARRS)

Exoplanets |

* HATS-36b
* KELT-18b
* Kepler-80g
* Kepler-90i
* LHS 1140 b
* Luyten b
* NGTS-1b
* OGLE-2016-BLG-1190Lb
* OGLE-2016-BLG-1195Lb
* Ross 128 b
* TRAPPIST-1e
* TRAPPIST-1f
* TRAPPIST-1g
* TRAPPIST-1h
* WASP-107b

Discoveries|

* GW170104
* GW170608
* GW170814
* GW170817
* Ring of Haumea
* IGR J17329-2731
* ʻOumuamua
* RZ Piscium
* ULAS J1342+0928
* Saraswati Supercluster

Space exploration|

* Cassini retirement

* Category:2016 in space — Category:2017 in space — Category:2018 in space

* v
* t
* e

2019 in space

* « 2018

2020 »

Space probe launches |

* Beresheet (lunar lander; Feb 2019)
* Chandrayaan-2 / Vikram / Pragyan (lunar obiter, lander and rover; Jul 2019)

Impact events|

* Kamchatka meteor (announced)
* 2019 MO

Selected NEOs|

* Asteroid close approaches
* 2016 AZ8
* 2018 XB4
* (12538) 1998 OH
* 66391 Moshup
* 1620 Geographos
* 2100 Ra-Shalom
* 2006 QV89
* 2019 SU3
* 2019 TA7
* 2019 UN13

Exoplanets |

* K2-288Bb
* Wolf 359 b and c
* Struve 2398 Bb and Bc
* Luyten's Star d and e
* L 1159-16 b, c, and d
* Gliese 687 c
* AD Leonis b
* Gliese 251 c
* LP 816-60 b
* Gliese 754 b
* Gliese 588 b and c
* Gliese 784 b
* Gliese 555 b
* Teegarden's Star b and c

Discoveries|

* 2019 AQ3
* ASASSN-19bt
* EPIC 204376071
* FarFarOut
* K2-18b water vapor detected on exoplanet
* Messier 87 supermassive black hole M87* imaged
* 2I/Borisov
* WD 0145+234 detection of exoasteroid disruption
* WD J0914+1914

Comets |

* 289P/Blanpain
* 78P/Gehrels
* 168P/Hergenrother
* 163P/NEAT
* 138P/Shoemaker–Levy
* 171P/Spahr

Space exploration|

* New Horizons (encounter with 486958 Arrokoth; Dec 2018 / Jan 2019)
* Chang'e 4 / Yutu-2 (landing on the far side of the Moon; Jan 2019)
* Hayabusa2 (departure from 162173 Ryugu; Dec 2019)

* Category:2018 in space — Category:2019 in space — Category:2020 in space

* v
* t
* e

2020 in space

* « 2019

2021 »

Space probe launches |

* Solar Orbiter (Feb 2020)
* Hope Mars Mission (Jul 2020)
* Tianwen-1 (Jul 2020)
* Mars 2020 (Jul 2020)
* Perseverance
* Mars Helicopter Ingenuity
* Chang'e 5 (lunar sample return mission; Oct 2020)

Selected NEOs|

* Asteroid close approaches
* 2020 BX12
* 2020 CD3 (temporary satellite)
* (52768) 1998 OR2
* 2020 JJ
* 2020 LD
* (163348) 2002 NN4
* 2011 ES4
* 2018 VP1
* (501647) 2014 SD224

Exoplanets |

* AU Mic b
* Gliese 229 Ac
* Gliese 433 (b * c * d)
* GJ 1151 b radio emissions
* Kepler-160d
* Kepler-1649c
* Lacaille 9352 (b * c)
* TOI 700 (b * c * d)
* TOI 732 (b * c)
* TOI 1338 b
* TOI 1339 (b * c * d)

Discoveries|

* 2020 AV2
* FRB 180916 source location and periodicity
* Radcliffe wave
* Ophiuchus Supercluster explosion
* PSO J03094+27
* 2MASS J10475385+2124234 wind speed measurements
* SGR 1935+2154
* HR 6819 black hole
* SWIFT J1818.0–1607
* South Pole Wall

Comets |

* C/2019 Y4 (ATLAS)
* C/2017 T2 (PANSTARRS)
* C/2020 F8 (SWAN)
* C/2019 U6 (LEMMON)
* C/2020 F3 (NEOWISE)
* 2P/Encke
* 88P/Howell

Space exploration|

* Spitzer retirement (Jan)
* BepiColombo (Earth gravity assist; Apr)
* OSIRIS-REx (collecting sample from asteroid Bennu; Oct)
* Hayabusa2 (sample return from asteroid Ryugu to Earth; Dec)

* Category:2019 in space — Category:2020 in space — Category:2021 in space

Coordinates:  01h 44m 04.0829s, −15° 56′ 14.928″

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Original source: https://en.wikipedia.org/wiki/Tau Ceti. Read more

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Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Tau_Ceti&oldid=4287713"
*[RA:]: Right Ascension
*[Dec.:]: Declination
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*[Primary]: Primary member of a system is the brightest one (and, in most cases, also the most massive one).