# TW Hydrae b

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Likely extrasolar planet in the constellation Hydra

TW Hydrae b Discovery Discovered by First: Setiawan et al. New study: Atacama Large Millimeter Array Discovery site First: Germany New study: Chile Discovery date First: December 2007 (disproven) New study: September 2016 Orbital characteristics Semi-major axis 22 AU (3.3×109 km) Star TW Hydrae Physical characteristics Mean radius ~4.25 R🜨 Mass 23.72[1] M🜨 Temperature ≥40 K (−233.2 °C; −387.7 °F)

**TW Hydrae b** is a likely Neptune-like [extrasolar planet](/source/Extrasolar_planet) orbiting at a distance of nearly 22 AU from the young [T Tauri star](/source/T_Tauri_star) [TW Hydrae](/source/TW_Hydrae) approximately 176 [light-years](/source/Light-year) (54 [parsecs](/source/Parsec), or nearly 1.665×1016 [km](/source/Km)) away in the [constellation](/source/Constellation) of [Hydra](/source/Hydra_(constellation)).

## Characteristics

### Mass, radius and temperature

TW Hydrae b is an [ice giant](/source/Ice_giant), an exoplanet with a radius and mass close to that of the ice giants [Neptune](/source/Neptune) and [Uranus](/source/Uranus). It may have an [equilibrium temperature](/source/Equilibrium_temperature) of around 40 K (−233.2 °C; −387.7 °F). It has an estimated mass of around 22.72 [M🜨](/source/Earth_mass) (or 1.5 *M*Neptune) and a possible radius of 4.25 [R🜨](/source/Earth_radius).

### Host star

The planet orbits a ([K-type](/source/Stellar_classification#Class_K)) [T Tauri star](/source/T_Tauri_star) named [TW Hydrae](/source/TW_Hydrae). The star has a mass of 0.8 [M☉](/source/Solar_mass) and a radius of 1.1 *R*☉. It has a temperature of 4000 [K](/source/Kelvin_scale) and is about 9 million years old. In comparison, the [Sun](/source/Sun) is 4.6 billion years old[2] and has a temperature of 5778 K.[3] Its luminosity ([L☉](/source/Solar_luminosity)) is 28% of that of the Sun.[note 1]

The star's [apparent magnitude](/source/Apparent_magnitude), or how bright it appears from Earth's perspective, is 11.27. Therefore, it is too dim to be seen with the naked eye.

### Orbit

TW Hydrae b orbits its host star at a distance of 22 AU (somewhat less than the orbital distance of [Neptune](/source/Neptune) from the Sun, which is 30.11 [AU](/source/Astronomical_unit)). The orbital period is not known, although taken its similar orbital distance as Neptune, the orbital period may be around the same value.

## Discovery

### First claims

In December 2007, a team led by Johny Setiawan of the [Max Planck Institute for Astronomy](/source/Max_Planck_Institute_for_Astronomy) in [Heidelberg](/source/Heidelberg), [Germany](/source/Germany) announced discovery of a planet orbiting TW Hydrae, dubbed "TW Hydrae b" with a minimum mass around 1.2 [Jupiter masses](/source/Jupiter_mass), a period of 3.56 days, and an orbital radius of 0.04 [astronomical units](/source/Astronomical_unit) (inside the inner rim of the protoplanetary disk). Assuming it orbited in the same plane as the outer part of the dust disk ([inclination](/source/Inclination) 7±1°[4]), it would have a true mass of 9.8±3.3 Jupiter masses.[4][5] However, if the inclination was similar to the inner part of the dust disk (4.3±1.0°[6]), the mass would be 16+5 −3 Jupiter masses, making it a [brown dwarf](/source/Brown_dwarf).[6] Since the star itself is so young, it was presumed this was the youngest extrasolar planet yet discovered, and essentially still in formation.[7] (only surpassed by [K2-33b](/source/K2-33b) and [V830 Tau b](/source/V830_Tau_b), both discovered nearly 9 years later).

### Disproven status

In 2008 a team of Spanish researchers concluded that the planet did not exist: the radial velocity variations were not consistent when observed at different [wavelengths](/source/Wavelength), which would not occur if the origin of the radial velocity variations was caused by an orbiting planet. Instead, the data was better modelled by [starspots](/source/Starspot) on TW Hydrae's surface passing in and out of view as the star rotates. "Results support the spot scenario rather than the presence of a hot Jupiter around TW Hya".[8] Similar wavelength-dependent radial velocity variations, also caused by starspots, have been detected on other T Tauri stars.[9]

### New proposal

In 2016, astronomers studying the protoplanetary disk of the star began to speculate why there was small dust grains in the gaps, including the one at 22 AU, but not large dust grains. Further investigations began to suggest that there may be a 1.5 *M*Neptune ice giant orbiting within the gap at 22 AU, which would be responsible for the observed gaps.

The study was then added to the online journal preprint archive [arXiv](/source/ArXiv) on September 1, 2016, gaining wide interest from media outlets.[1]

## Notes

1. **[^](#cite_ref-4)** From L = 4 π R 2 σ T e f f 4 {\displaystyle {\begin{smallmatrix}L=4\pi R^{2}\sigma T_{\rm {eff}}^{4}\end{smallmatrix}}} , where L {\displaystyle {\begin{smallmatrix}L\end{smallmatrix}}} is the luminosity, R {\displaystyle {\begin{smallmatrix}R\end{smallmatrix}}} is the radius, T e f f {\displaystyle {\begin{smallmatrix}T_{\rm {eff}}\end{smallmatrix}}} is the effective surface temperature and σ {\displaystyle {\begin{smallmatrix}\sigma \end{smallmatrix}}} is the [Stefan–Boltzmann constant](/source/Stefan%E2%80%93Boltzmann_constant).

## References

1. ^ [***a***](#cite_ref-Tsukagoshi_1-0) [***b***](#cite_ref-Tsukagoshi_1-1) Tsukagoshi, Takashi; Nomura, Hideko; Muto, Takayuki; Kawabe, Ryohei; Ishimoto, Daiki; Kanagawa, Kazuhiro D.; Okuzumi, Satoshi; Ida, Shigeru; Walsh, Catherine; Millar, Tom J. (2016). ["A Gap with a Deficit of Large Grains in the protoplanetary disk around TW Hya"](https://doi.org/10.3847%2F2041-8205%2F829%2F2%2FL35). *The Astrophysical Journal*. **829** (2): L35. [arXiv](/source/ArXiv_(identifier)):[1605.00289](https://arxiv.org/abs/1605.00289). [Bibcode](/source/Bibcode_(identifier)):[2016ApJ...829L..35T](https://ui.adsabs.harvard.edu/abs/2016ApJ...829L..35T). [doi](/source/Doi_(identifier)):[10.3847/2041-8205/829/2/L35](https://doi.org/10.3847%2F2041-8205%2F829%2F2%2FL35). [S2CID](/source/S2CID_(identifier)) [41738556](https://api.semanticscholar.org/CorpusID:41738556).

1. **[^](#cite_ref-2)** Fraser Cain (16 September 2008). ["How Old is the Sun?"](http://www.universetoday.com/18237/how-old-is-the-sun/). [Universe Today](/source/Universe_Today). Retrieved 19 February 2011.

1. **[^](#cite_ref-3)** Fraser Cain (15 September 2008). ["Temperature of the Sun"](http://www.universetoday.com/18092/temperature-of-the-sun/). Universe Today. Retrieved 19 February 2011.

1. ^ [***a***](#cite_ref-setiawan08_5-0) [***b***](#cite_ref-setiawan08_5-1) Setiawan, J.; Henning, Th.; Launhardt, R.; Müller, A.; Weise, P.; Kürster, M. (3 January 2008). "A young massive planet in a star–disk system". *Nature*. **451** (7174): 38–41. [Bibcode](/source/Bibcode_(identifier)):[2008Natur.451...38S](https://ui.adsabs.harvard.edu/abs/2008Natur.451...38S). [doi](/source/Doi_(identifier)):[10.1038/nature06426](https://doi.org/10.1038%2Fnature06426). [PMID](/source/PMID_(identifier)) [18172492](https://pubmed.ncbi.nlm.nih.gov/18172492). [S2CID](/source/S2CID_(identifier)) [4431370](https://api.semanticscholar.org/CorpusID:4431370).

1. **[^](#cite_ref-newscientist_6-0)** McKee, Maggie (2 January 2008). ["First planet discovered around a youthful star"](https://www.newscientist.com/article/dn13135-first-planet-discovered-around-a-youthful-star.html). NewScientist.com news service. Retrieved 2008-01-02.

1. ^ [***a***](#cite_ref-pontoppidan08_7-0) [***b***](#cite_ref-pontoppidan08_7-1) Pontoppidan, Klaus M.; et al. (2008). "Spectro-astrometric imaging of molecular gas within protoplanetary disk gaps". *[The Astrophysical Journal](/source/The_Astrophysical_Journal)*. **684** (2): 1323–1329. [arXiv](/source/ArXiv_(identifier)):[0805.3314](https://arxiv.org/abs/0805.3314). [Bibcode](/source/Bibcode_(identifier)):[2008ApJ...684.1323P](https://ui.adsabs.harvard.edu/abs/2008ApJ...684.1323P). [doi](/source/Doi_(identifier)):[10.1086/590400](https://doi.org/10.1086%2F590400). [S2CID](/source/S2CID_(identifier)) [15445587](https://api.semanticscholar.org/CorpusID:15445587).

1. **[^](#cite_ref-mpia_8-0)** ["A young extrasolar planet in its cosmic nursery: Astronomers from Heidelberg discover planet in a dusty disk around a newborn star"](http://www.mpia.de/Public/menu_q2e.php?Aktuelles/PR/2008/PR080103/PR_080103_en.html). [Max Planck Institute for Astronomy](/source/Max_Planck_Institute_for_Astronomy). 2008-01-02. Retrieved 2008-01-03.

1. **[^](#cite_ref-huelmo_9-0)** Huelamo, N.; et al. (2008). "TW Hydrae: evidence of stellar spots instead of a Hot Jupiter". *[Astronomy and Astrophysics](/source/Astronomy_and_Astrophysics)*. **489** (2): L9–L13. [arXiv](/source/ArXiv_(identifier)):[0808.2386](https://arxiv.org/abs/0808.2386). [Bibcode](/source/Bibcode_(identifier)):[2008A&A...489L...9H](https://ui.adsabs.harvard.edu/abs/2008A&A...489L...9H). [doi](/source/Doi_(identifier)):[10.1051/0004-6361:200810596](https://doi.org/10.1051%2F0004-6361%3A200810596). [S2CID](/source/S2CID_(identifier)) [18775872](https://api.semanticscholar.org/CorpusID:18775872).

1. **[^](#cite_ref-prato_10-0)** Prato, L.; et al. (2008). "A Young Planet Search in Visible and IR Light: DN Tau, V836 Tau, and V827 Tau". *[The Astrophysical Journal](/source/The_Astrophysical_Journal)*. **687** (2): L103–L106. [arXiv](/source/ArXiv_(identifier)):[0809.3599](https://arxiv.org/abs/0809.3599). [Bibcode](/source/Bibcode_(identifier)):[2008ApJ...687L.103P](https://ui.adsabs.harvard.edu/abs/2008ApJ...687L.103P). [doi](/source/Doi_(identifier)):[10.1086/593201](https://doi.org/10.1086%2F593201). [S2CID](/source/S2CID_(identifier)) [14888302](https://api.semanticscholar.org/CorpusID:14888302).

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Adapted from the Wikipedia article [TW Hydrae b](https://en.wikipedia.org/wiki/TW_Hydrae_b) by Wikipedia contributors ([contributor history](https://en.wikipedia.org/wiki/TW_Hydrae_b?action=history)). Available under [Creative Commons Attribution-ShareAlike 4.0 International](https://creativecommons.org/licenses/by-sa/4.0/). Changes may have been made.