HAT-P-1 b
Extrasolar planet List of extrasolar planets
Size comparison of HAT-P-1b with Jupiter.
Parent star

<tr> <td colspan="2">Star</td> <td>HAT-P-1 (ADS 16402 B)</td></tr><tr> <td colspan="2">Constellation</td> <td>Lacerta</td></tr><tr> <td>Right ascension</td> <td style="text-align: center">(α)</td> <td>22h 57m 47s</td></tr><tr> <td>Declination</td> <td style="text-align: center">(δ)</td> <td>+38° 40′ 30″</td></tr><tr><td colspan="2">Distance</td><td>453 ± 65 ly
(139 ± 20 pc)</td></tr><tr><td colspan="2">Spectral type</td> <td>G0V [1]</td></tr>

Orbital elements

<tr><td>Semimajor axis</td><td style="text-align: center">(a)</td> <td>0.0553 ± 0.0014[2] AU</td></tr><tr> <td>Eccentricity</td> <td style="text-align: center">(e)</td> <td><0.067[2]</td></tr><tr><td>Orbital period</td><td style="text-align: center">(P)</td> <td>4.4652934 ± 0.0000093[2] d</td></tr><tr><td> </td> <td style="text-align: center"> </td> <td>(107.16704 h)</td></tr><tr> <td>Inclination</td> <td style="text-align: center">(i)</td> <td>86.28 ± 0.20[2]°</td></tr><tr> <td>Time of transit</td> <td style="text-align: center">(Tt)</td> <td>2,454,363.94656 ± 0.00072[2] JD</td></tr><tr> <td>Semi-amplitude</td> <td style="text-align: center">(K)</td> <td>59.3 ± 1.4[2] m/s</td></tr>

Physical characteristics

<tr><td>Mass</td><td style="text-align: center">(m)</td><td>0.524 ± 0.031[2] MJ</td></tr><tr><td>Radius</td><td style="text-align: center">(r)</td><td>1.225 ± 0.059 [2] Template:Jupiter radius</td></tr>

Discovery information

<tr> <td colspan="2">Discovery date</td> <td>Thurs, Sept 14, 2006</td></tr><tr> <td colspan="2">Discoverer(s)</td> <td>HATNet Project</td></tr><tr> <td colspan="2">Discovery method</td> <td>Transit, radial velocity</td></tr><tr> <td colspan="2">Discovery site</td> <td>Arizona and Hawaii</td></tr><tr> <td colspan="2">Discovery status</td> <td>Published</td></tr>

HAT-P-1b is an extrasolar planet orbiting the Sun-like star HAT-P-1, also known as ADS 16402 B. HAT-P-1 is the dimmer component of the ADS 16402 binary star system. It is located 453 light years away from Earth in the constellation Lacerta. HAT-P-1b is among the least dense of any of the known extrasolar planets.

Discovery Edit

HAT-P-1b was detected by searching for astronomical transits of the parent star by orbiting planets. As the planet passes in front of its parent star (as seen from Earth), it blocks a small amount of the light reaching us from the star. HAT-P-1b was first detected by a dip of 0.6% in the light from the star. This enabled determination of the planet's radius and orbital period. The discovery was made by the HATNet Project (Hungarian Automated Telescope Network) using telescopes in Arizona and Hawaii and announced on September 14, 2006.[3]

Orbit and mass Edit

HAT-P-1b is located in a very close orbit to its star, taking only 4.47 days to complete.[1] It therefore falls into the category of hot Jupiters. At only 8.27 million kilometers from the star, tidal forces would circularise the orbit unless another perturbing body exists in the system. At the present time, the existing measurements are not sufficient to determine the orbital eccentricity, so a perfectly circular orbit has been assumed by the discoverers.[4] However, the eccentricity of the planet was calculated to be no greater than 0.067.

In order to determine the mass of the planet, measurements of the star's radial velocity variations were made by the N2K Consortium. This was done by observing the Doppler shift in the star's spectrum. Combined with the known inclination of the orbit as determined by the transit observations, this revealed the mass of the planet to be 0.53±0.04 times that of Jupiter.[1]


As of August 2008, the most recent calculation of HAT-P-1b's Rossiter-McLaughlin effect and so spin-orbit angle was that of Johnson.[5] This is +3.6 ± 2.0 degrees.[2]

Characteristics Edit

As evidenced by its high mass and planetary radius, HAT-P-1b is a gas giant, most likely composed primarily of hydrogen and helium. The planet would thus have no well-defined surface. Current theories predict that such planets formed in the outer regions of their solar systems and migrated inwards to their present orbits.

HAT-P-1b is significantly larger than predicted by theoretical models.[3] This may indicate the presence of an additional source of heat within the planet. One possible candidate is tidal heating from an eccentric orbit, a possibility which has not been ruled out from the available measurements.[6] However, another planet with a significantly inflated radius, HD 209458 b, is in a circular orbit.

An alternative possibility is that the planet has a high axial tilt, like Uranus in our solar system. The problem with this explanation is that it is thought to be quite difficult to get a planet into this configuration, so having two such planets among the set of known transiting planets is problematic.

References Edit

  1. 1.0 1.1 1.2 (2007). HAT-P-1b: A Large-Radius, Low-Density Exoplanet Transiting One Member of a Stellar Binary. The Astrophysical Journal 656 (1): 552–559.
  2. 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 (2008). Measurement of the Spin-Orbit Angle of Exoplanet HAT-P-1b. The Astrophysical Journal 686 (1): 649–657.
  3. 3.0 3.1 Oversize Orb: Puffy planet poses puzzle. Science News Online. Archived from the original on 2007-10-13. Retrieved 2007-10-14.
  4. A HAT trick. Retrieved 2007-10-14.
  5. (2008). Measuring accurate transit parameters. Proceedings of the International Astronomical Union 4: 99.
  6. Jackson, Brian (2008). Tidal Heating of Extra-Solar Planets. ApJ 681 (2): 1631.

External linksEdit


Coordinates: Sky map 22h 57m 47s, +38° 40′ 30″

Ad blocker interference detected!

Wikia is a free-to-use site that makes money from advertising. We have a modified experience for viewers using ad blockers

Wikia is not accessible if you’ve made further modifications. Remove the custom ad blocker rule(s) and the page will load as expected.