HD4208

HD 40979 b is an extrasolar planet orbiting the star HD 40979, was detected from the Lick and Keck observatories and photometric observations at Fairborn Observatory reveal low-amplitude brightness variations in HD 40979. It is thought to be a large gas giant planet. It was discovered in 2002 by Debra Fischer.

M1.5II-III

Confirmed

HD 37646 is a double star in the northern constellation of Auriga. The pair have an angular separation of 26.005″.

HIP+3502

K3V

Vogt, et al.

using HARPS

HD 4313 b is an extrasolar planet orbiting the G-type star HD 4313 approximately 447 light years away in the constellation Pisces.

K2 III

HD 4308 b is a low-mass exoplanet orbiting around HD 4308. It is believed to have almost no orbital eccentricity.

HD 44780 B

HD 45350 b is an extrasolar planet located approximately 160 light-years away in the constellation of Auriga. It has a minimum mass about 1.79 times that of Jupiter. The mean distance of the planet from the star is more than the distance between Mars and the Sun, but the eccentricity of the orbit is nothing short of remarkable; at periastron the planet is as close to the star as Mercury is from the Sun, but at apastron it is 8 times further. No doubt seasons on the planet would be extreme.Dynamical simulations covering a period of 107 years show that a second, low-mass, planet could only orbit stably if it were no more than 0.2 AU away from the star; in the simulations, these planets show oscillations in eccentricity up to an eccentricity of 0.25. Radial velocity observations rule out any such planet whose mass is greater than 4 Neptune masses.

HD 37124c

HD 40307 d is an extrasolar planet orbiting the star HD 40307, located 42 light-years from Earth in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the HARPS apparatus in June 2008. It is the most massive of the six proposed planets in the system. The planet is of interest as this star has relatively low metallicity, supporting a hypothesis that different metallicities in protostars determine what kind of planets they will form.

HD 4113 is an 8th magnitude metal rich G5V star located approximately 144 light-years away in the constellation Sculptor. This star is similar to our Sun and has one known planet.

HD 37124 c

Zucker et al.

Mikko Tuomi et al.

HD 40307 is an orange (K-type) main-sequence star located approximately 42 light-years away in the constellation of Pictor (the Easel), taking its primary name from its Henry Draper Catalogue designation. It is calculated to be slightly less massive than the Sun. HD 40307 was observed during or before 1900 as part of the Cape Photographic Durchmusterung. The star has six known planets, three discovered in 2008 and three more in 2012. One of them, HD 40307 g, is a potential super-Earth in the habitable zone, with an orbital period of about 200 days. This object might be capable of supporting liquid water on its surface, although much more information must be acquired before its habitability can be assessed.

HD 43587 is a stellar system approximately 63 light-years away in the constellation of Orion, visible to the naked eye. The system comprises four individual stars, with two widely separated binaries forming a quadruple system.

radial velocity, using HARPS

HD 40307 f

K0V

G6V

HD 4113 b is a jovian planet located approximately 144 light-years away in the constellation of Sculptor, orbiting the star HD 4113. This planet has a very eccentric orbit with a 527-day period at 1.28 AU from the parent star. At periastron, the distance is 0.124 AU and at apastron, the distance is 2.44 AU.

HD 41004 Ab
yes

HD 40307 is an orange (K-type) main-sequence star located approximately 42 light-years away in the constellation of Pictor (the Easel), taking its primary name from its Henry Draper Catalogue designation. It is calculated to be slightly less massive than the Sun. HD 40307 was observed during or before 1900 as part of the Cape Photographic Durchmusterung. The star has six known planets, three discovered in 2008 and three more in 2012.

HD 40979 is a yellow-white dwarf star about 108 light-years away in the constellation of Auriga. The star is a member of a multiple system: it has a companion HD 40979B which shares its proper motion and is located at a projected distance of 6400 AU from the primary. HD 40979B itself has a companion (designated HD 40979C) at a projected distance of 129 AU from star B, making the system a triple.As of 2002, there is one extrasolar planet known to be orbiting around HD 40979A.

HD 44594 is a star in the southern constellation Puppis. It has an apparent visual magnitude of 6.64, so it can be seen with the naked eye from the southern hemisphere under good viewing conditions. Based upon parallax measurements, it is located at a distance of about 82 light-years (25 parsecs) from the Earth, giving it an absolute magnitude of 4.56.Measurement of the star's spectrum show it to match a stellar classification of G1.5V, which is close to the Sun's spectral class of G2V.

HD 43691 is a G-type star with magnitude +8.03 located approximately 260 light-years away in the constellation Auriga. This yellow star is about to stop thermonuclear hydrogen-fusion in its core and eventually expand to become a red giant.

Orion

HD 43587 BC

HD 40307 e is an extrasolar planet orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Obervatory's HARPS apparatus by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Goettingen, Germany.Its minimum mass is 3.5 that of Earth - the smallest - and dynamical models suggest it cannot be much more (and so is measured close to edge-on). It further gets roughly the same insolation from its star as Mercury gets from the Sun. Planets like this in that system have been presumed "super-Earth".However planets b, c, and d are presumed to have migrated in from outer orbits; and planet b is predicted a sub-Neptune. It is likely that this planet formed even further out. Whether it is a sub-Neptune, a super-Venus or even a super-Mercury is unknown.

HD 40307 g

HD 40979 b

HD 4308 b

K2-3III

G9IV/V

Tamuz et al.

HD 38529 A

HD 38283 b is an extrasolar planet, orbiting the 7th magnitude F-type main-sequence star HD 38283, 123 light years away in the constellation Mensa. It is a Saturn-like planet orbiting at Earth-like distance in the middle of its habitable zone. But its eccentricity is 0.41, much higher than the Earth's eccentricity of 0.017. The planet's distance ranges from about 0.60 AU (closer to its star than Venus is to the Sun) and 1.44 AU (nearly as distant from its star as Mars is to the Sun).

K2.5V

HD 38283 b

HD 38529 b

Vogt et al.

Correia et al.

HIP 29860, Gliese 231.1, HR 2251

HD 37646 A

HD 38529 d

B2IV-V

HD 40307 b

HD4203

HD 37124 d is an extrasolar planet approximately 108 light-years away in the constellation of Taurus. The planet was discovered in 2005 orbiting the star HD 37124 in a long-period orbit. Based on its mass, it is considered to be a gas giant. An alternative solution to the radial velocities gives a period of 29.92 days and a minimum mass 17% that of Jupiter.

HD 4308

HD 44780 A

HD 43587 Ab

Published

HD 4502

HD 4308 is a 6th magnitude star located approximately 72 light years away in the southern constellation of Tucana.

Marcy et al.

HD 43197 b is an extrasolar planet which orbits the G-type main sequence or subgiant star HD 43197, located approximately 180 light years away in the constellation Canis Major. This planet has at least three-fifths the mass of Jupiter and takes 0.9 years to orbit the star at a semimajor axis of 0.868 AU. However unlike most other known exoplanets, its eccentricity is not known, but it is typical that its inclination is not known.

HD 37124 d

B0.5Ia+

G9V
HD 45364 b is an extrasolar planet located approximately 107 light years away in the constellation of Canis Major, orbiting the 8th magnitude G-type main sequence star HD 45364. Its minimum mass is 63% that of Saturn or 19% that of Jupiter. It takes 227 days to orbit the star at a distance 68% that of Earth’s distance from the Sun. This planet was discovered by HARPS on August 8, 2008 and announced together with HD 45364 c. It is located in a 3:2 orbital resonance with HD 45364 c.

WDS J06173+0506Aa,Ab, LEP 24A

B9.5III-IV.

B2.5V

HD 40307 c

G4V

HD 41742 AabB/HD 41700 (C)

HD 38858 is a G-type star with one detected planet. The planet, designated HD 38858 b, is about twice the mass of Uranus and orbits in the star's habitable zone.The last observation of this system for a dust disc or comet belt was in 2009 by the Spitzer Space Telescope; a belt was inferred at 102 AU. It has an inclination of 48◦.

HD 4203 b is an exoplanet more massive than Jupiter. It orbits two times further from the star than Earth to the Sun. The planet takes 1.1824 year to orbit the star very eccentrically from 1.00 AU to 3.14 AU. The planet was discovered by Steve Vogt using the Keck telescope.

HD 4113 b

G5 D

Udry et al.

HD 4391 is a triple star system in the constellation Phoenix that is located at a distance of 48.7 light years from the Sun. The primary has a stellar classification of G3V, which is a G-type main sequence star. The physical properties of this star are similar to the Sun, making it a solar analog. However, it is believed to have 22% greater mass than the Sun and is only 1.2 billion years old.

HD 40307 g is an exoplanet orbiting in the habitable zone of HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Observatory's HARPS apparatus by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Goettingen, Germany.

HD 41742 B

HD 4313 b

HIP 28393 b

HD 37605 is an orange dwarf star located approximately 143 light years away in the constellation Orion. It formed about 7 billion years ago and is inactive.There are two giant planets known in orbit. Planet b was discovered in 2004 and planet c was discovered eight years later.

HD 39225, also known as HR 2028, is a variable star in the constellation Auriga. A red giant star, it is suspected of varying in brightness between magnitudes 5.82 and 6.07. Located around 800 light-years distant, it shines with a luminosity approximately 595 times that of the Sun and has a surface temperature of 3900 K.

G0V / M0V / M3.5V / M5V

HD 41162 is star in double system.

HD 37756 is a class B2IV (blue subgiant) star in the constellation Orion. Its apparent magnitude is 4.95 and it is approximately 900 light years away based on parallax.It is a spectroscopic binary, with a period of 27 days and eccentricity 0.72.

HD 38529 c

HD 42540, also known as HR 2196, is a suspected variable star in the constellation Pictor. A class K2-3III orange giant, its apparent magnitude is 5.04 and it is approximately 362 light years away based on parallax.

radial velocity

HD 38282 (R144, BAT99-118, Brey 89) is a massive spectroscopic binary star in the Tarantula Nebula (Large Magellanic Cloud), consisting of two hydrogen-rich Wolf-Rayet stars.R144 is located near the R136 cluster at the center of NGC 2070 and may have been ejected from it after an encounter with another massive binary.Both components of R144 are detected in the spectrum and both are WNh stars, very hot stars with strong emission lines due to their strong stellar winds. The orbit has not been determined, but is likely to be between two and six months long, possibly more if it is eccentric. The primary, slightly hotter, star is observed to be the less massive of the two.Each star is amongst the most luminous known, but the exact parameters of each has not been determined. Their combined luminosity is around 4,500,000 L☉ to 6,300,000 L☉. The masses have not yet been calculated accurately from the orbital parameters, but the stars have been modelled to initially have been around 260 M☉ and 175 M☉. Depending on their exact age, this has now decreased to between 90 M☉ and 170 M☉ for the primary and 95 M☉ and 205 M☉ for the secondary.

HD 38283 b is an extrasolar planet, orbiting the 7th magnitude F-type main-sequence star HD 38283, 123 light years away in the constellation Mensa. It is a Saturn-like planet orbiting at Earth-like distance in the middle of its habitable zone. But its eccentricity is 0.41, much higher than the Earth's eccentricity of 0.017. The planet's distance ranges from about 0.60 AU (closer to its star than Venus is to the Sun) and 1.44 AU (nearly as distant from its star as Mars is to the Sun). This planet takes 363.2 days to orbit the star, just two days shy of the Earth's orbital period of 365.256366 days. Its mass is one-thirds that of Jupiter but its size and density are not known. Since inclination is not known, its actual mass is unknown, either slightly greater or much greater than its lower limit.This planet may have Earth-like moons with bodies of water and possibly life. But giving the planet's high eccentricity, life on the moons may not evolve as well as those on Earth. From the surface of the moon, ones may see parent planet in the sky about half of the times with different phases just like the Moon seen from Earth, as well as other moons. If this planet has rings nearly as prominent as Saturn's, then the rings can be seen surrounding the planet, making this scenery even more amazing.HD 38283 b was discovered on 11 April 2011 using the radial velocity technique using the Anglo-Australian Telescope (AAT). This method uses to look for planets by watching the star periodically wobble caused by the gravitational tug of the orbiting planets.

HD 43587 B

HD 37605c

Announced

HD 45364 is a star approximately 107 light years away from Earth in the constellation of Canis Major. As of August 2008 there are two confirmed extrasolar planets orbiting around it.

HD4113

HD 45184 is a 6th magnitude G-type main sequence star located approximately 71 light years away in the constellation Canis Major. It has a planet around 12 times as massive as Earth that takes 5.88 days to complete an orbit around its host star. The planet was detected by radial velocity.

HD 38529 b is an extrasolar planet approximately 138 light years away in the constellation of Orion. This planet was discovered in 2000. Because of its mass, it is likely that it is a gas giant.

HD 45350 is an 8th magnitude star located approximately 160 light-years away in the constellation of Auriga. It is a yellow subgiant (spectral type G5 IV), a Sun-like star that is finishing hydrogen fusion in its core. Although slightly cooler, it is brighter, although not much considering its subgiant status. However, the star is very old and will soon start to expand becoming finally a red giant.

HD 43848 is a 9th magnitude K-type subgiant star located approximately 123 light-years away in the constellation of Columba. The star is less massive than the Sun.On October 29, 2008, radial velocity measurements made with the MIKE echelle spectrograph on the 6.5-m Magellan II (Clay) telescope revealed the presence of a companion of at least 25 Jupiter masses orbiting the star. Initially thought to be a brown dwarf, astrometric measurements reveal that the true mass of the object is 120+167−43 Jupiter masses, implying that it is likely to be a red dwarf star.

HD 41742/41700 is a star system that lies approximately 87 light-years away in the constellation of Puppis. The system consists of two bright stars where the primary is orbited by two fainter stars, making it a quadruple with an unequal hierarchy.

HD 40307 d

HD 43587 C

−0.88

HD 43587 Aa

HD 38283 is a 7th magnitude F-type main sequence star located approximately 125 light-years away in the constellation of Mensa. HD 38283 is not visible to the naked eyes for most people but can be easily seen using binoculars.

HD 38529b

HD 38529 B

Naef et al.

HD 44627A

G5V

HR 2209, HD 42818, HIP 29997, SAO 13788

HD 40307 f is an extrasolar planet orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Obervatory's HARPS apparatus by a team of astronomers led by Mikko Tuomi at the University of Hertfordshire and Guillem Anglada-Escude of the University of Goettingen, Germany.This planet is the fifth planet from the star, at a distance of about 0.25 AU (compared to 0.39 AU for Mercury) with negligible eccentricity.HD 40307 f's minimum mass is 5.2 that of Earth, and dynamical models suggest it cannot be much more (and so is measured close to edge-on). Planets like this in that system have been presumed "super-Earth".Even though HD 40307 f is closer to the star than Mercury is to the Sun, it gets (slightly) less insolation than Mercury gets because the parent star is dimmer than our home star. It still gets more heat than Venus gets (like Gliese 581 c), and it has more gravitational potential than Venus has. HD 40307 f is more likely a super-Venus than a "super-Earth".Moreover, planets b, c, and d are presumed to have migrated in from outer orbits; and planet b is predicted a sub-Neptune. It is likely that this planet f formed even further out. Whether it is a sub-Neptune or super-Venus is, perhaps, a moot point.

HD 40307b

HD 39091 b

HD 44131 is a class M1III (red giant) star in the constellation Orion. Its apparent magnitude is 4.91 and it is approximately 465 light years away based on parallax.

HD 45364 b

HD 43691 b is a massive jovian planet located approximately 260 light-years away in the constellation of Auriga. Because the inclination is unknown, only the minimum mass is known. The planet orbits close to the star, closer than Mercury to the Sun.

HD 37124d

HD 37124 c is an extrasolar planet approximately 108 light-years away in the constellation of Taurus. The planet was discovered in 2002 orbiting the star HD 37124. The planet is most likely to be a gas giant (based on its mass).

HD 4208 is an 8th magnitude star located approximately 106 light years away in the constellation of Sculptor. Its spectral type is G5V. It is a yellow dwarf similar to our Sun, only slightly cooler and dimmer. It is not visible to the unaided eye, but with binoculars or small telescope it should be an easy target.In 2001, a planet was discovered orbiting the star.

HD 43197b

HD 44780 is a star in the Henry Draper Catalogue. It is a spectroscopic binary star, located about 3° north of Mu Geminorum. It is composed of two giant stars, orbiting each other with a period of 577 days. This type of binary system is relatively rare.

HD 400

G0IV-V

HD 4208 b

HD 41004 Ab is an extrasolar planet approximately 139 light years away in the constellation of Pictor. It has mass 2.56 MJ planet orbiting at a distance of 1.70 AU from HD 41004 A. The planet's orbit is highly eccentric caused by the companion star HD 41004 B and the distance ranges from 0.44 to 2.96 astronomical units.

Tinney et al.

HD 41004 B b

HD 38282 (R144, BAT99-118, Brey 89) is a massive spectroscopic binary star in the Tarantula Nebula (Large Magellanic Cloud), consisting of two hydrogen-rich Wolf-Rayet stars.R144 is located near the R136 cluster at the center of NGC 2070 and may have been ejected from it after an encounter with another massive binary.Both components of R144 are detected in the spectrum and both are WNh stars, very hot stars with strong emission lines due to their strong stellar winds.

California, United States

HD 37605 c

G8III + F0V:

HD 40307c

NLTT 16333, WDS J06173+0506E, LEP 24AE

Mayor et al.

HD 4391

Disk

HD 38529 Ab

HD 44219 is an 8th magnitude G-type main sequence star located approximately 164 light years away in the constellation Monoceros. This star is larger, cooler, brighter, and about the same mass as our Sun. Also its metal content is one-fifteenth more than the Sun. In 2009, a gas giant planet was found in orbit around the star.

HD 37605 is an orange dwarf star located approximately 143 light years away in the constellation Orion. It formed about 7 billion years ago and is inactive.There are two giant planets known in orbit. Planet b was discovered in 2004 and planet c was discovered eight years later. The planets do not transit relative to Earth; b's maximum inclination is 88.1%.In a simulation, HD 37605 b's orbit "sweeps clean" most test particles within 0.5 AU; leaving only asteroids "in low-eccentricity orbits near the known planet’s apastron distance, near the 1:2 mean-motion resonance" with oscillating eccentricity up to 0.06, and also at 1:3 with oscillating eccentricity up to 0.4. Also, observation has ruled out planets heavier than 0.7 Jupiter mass with a period of one year or less; which still allows for planets at 0.8 AU or more.

F9.5V

F7.5V

A0Vn

HD 43587 Aab

K2 IV

HD 40409 is a star in the constellation Dorado. Its apparent magnitude is 4.66.

HD 40307 f is an extrasolar planet orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor.

HD 45350 b is an extrasolar planet located approximately 160 light-years away in the constellation of Auriga. It has a minimum mass about 1.79 times that of Jupiter. The mean distance of the planet from the star is more than the distance between Mars and the Sun, but the eccentricity of the orbit is nothing short of remarkable; at periastron the planet is as close to the star as Mercury is from the Sun, but at apastron it is 8 times further.

HD 41004 Bb

HD 4203b

HD 4113b

HD 40307 e

HD 43197 b is an extrasolar planet which orbits the G-type main sequence or subgiant star HD 43197, located approximately 180 light years away in the constellation Canis Major. This planet has at least three-fifths the mass of Jupiter and takes 0.9 years to orbit the star at a semimajor axis of 0.868 AU. However unlike most other known exoplanets, its eccentricity is not known, but it is typical that its inclination is not known. This planet was detected by HARPS on October 19, 2009, together with 29 other planets.

HD 37519 is star in the northern constellation Auriga. It is chemically peculiar, showing an abnormal level of mercury in the spectrum.

The extrasolar planet, designated as HD 4208 b, was discovered by the California and Carnegie Planet Search team using the Keck telescope. The planet is probably somewhat less massive than Jupiter, although only its minimum mass is known. Its orbital distance is 1.67 AU, slightly further than Mars and its eccentricity is low.

HD 43848 is a 9th magnitude K-type subgiant star located approximately 123 light-years away in the constellation of Columba. The star is less massive than the Sun.On October 29, 2008, radial velocity measurements made with the MIKE echelle spectrograph on the 6.5-m Magellan II (Clay) telescope revealed the presence of a companion of at least 25 Jupiter masses orbiting the star.

HD 41742 Aab

HD 40979b

HD 41742 AabB

SAO 217660 b

HD 43197 b

HD 41248 is a star in the constellation Pictor. It is a star very similar to our Sun, with the same spectral type (G2V). It has 68% of the Sun's luminosity, 92% of its mass and 78% of its diameter. It is estimated to be around 2 billion years old, and it has a lower metallicity—43% that of the Sun.

HD 37605b

Da Silva et al.

HD 41248 is a star in the constellation Pictor. It is a star very similar to our Sun, with the same spectral type (G2V). It has 68% of the Sun's luminosity, 92% of its mass and 78% of its diameter. It is estimated to be around 2 billion years old, and it has a lower metallicity—43% that of the Sun. With an apparent visual magnitude of 8.81, it is too faint to be seen with the unaided eye, and is located around 170 light-years (52 parsecs) away from the Solar System.HD 41248 was investigated in the High Accuracy Radial Velocity Planet Searcher (HARPS) and initially thought not to have planets, but review of its spectrum showed it to have two super-earths with orbital periods of 18.357 days and 25.648 days and minimum masses 12.3 and 8.6 times that of the Earth. The planets are in a 7:5 mean motion resonance. The existence of the planets has been called into question as being a possible false detection due to stellar activity, with a cycle of 25 days related to the star's rotational period. The original researchers conceded small planet signals could be difficult to unravel from signal noise and noted that the star had become more active in recent years, but in reanalysing all the data concluded that the stability of the radial velocity signals over ten years strengthened the case for the planet hypothesis. They add that more conclusive proof could come as instruments operating in the near infrared such as CARMENES or the Habitable Zone Planet Finder (HPF) become operational.

HD 37605 b is an extrasolar planet that has nearly three times more mass than Jupiter. It orbits close to the star, taking 54 days to revolve around the parent star HD 37605. Its orbit is highly eccentric, around 74%. Distance from HD 37605 ranges from 0.069 to 0.453 astronomical units.It is the first planet found by Hobby-Eberly Telescope (HET) in July 2004.In a simulation, HD 37605 b's orbit "sweeps clean" most test particles within 0.5 AU; leaving only asteroids "in low-eccentricity orbits near the known planet’s apastron distance, near the 1:2 mean-motion resonance" with oscillating eccentricity up to 0.06, and also at 1:3 with oscillating eccentricity up to 0.4.

HD 40873 is a star in the northern constellation of Auriga. Located around 440 light-years distant, it shines with a luminosity approximately 38 times that of the Sun and has a surface temperature of 7,753 K. It is a suspected variable star.Samuel Molyneux named this star Telescopica in Auriga. Flamsteed catalogued it as 35 Camelopardali Heveliana, which is the name James Bradley continued to use, although it is within the borders of the modern constellation Auriga. Francis Baily reclassified it to Auriga as star 1924 in the British Association's 1845 Catalogue of 8377 Stars.

Howard et al.

HD 43

HD 43197 is a 9th magnitude G-type main sequence or subgiant star located approximately 180 light years away in the constellation Canis Major. This star is larger, cooler, fainter, and less massive than our Sun. Also its metal content is five halves as much as the Sun. In 2009, a gas giant planet was found in orbit around the star.

HD 45350 b

HD 44219 b

HD 4203

HD 43848 b

HD 38529c

HD 43691 b

HD 38858 b

K2III

G1.5V

HD 4203 is a 9th magnitude star located approximately 250 light years away in the constellation Pisces. The star is yellow with spectral type G5. The star has evolved for 9.41 billion years. The star has a gas giant planet orbiting around a high metallicity star.

HD 40657 is a class K1.5III (orange giant) star in the constellation Orion. Its apparent magnitude is 4.52 and it is approximately 420 light years away based on parallax.

HD 44594 is a star in the southern constellation Puppis. It has an apparent visual magnitude of 6.64, so it can be seen with the naked eye from the southern hemisphere under good viewing conditions. Based upon parallax measurements, it is located at a distance of about 82 light-years (25 parsecs) from the Earth, giving it an absolute magnitude of 4.56.Measurement of the star's spectrum show it to match a stellar classification of G1.5V, which is close to the Sun's spectral class of G2V. In the wavelength range 3200–8800 Â, the energy emission of this star is very similar to the Sun, and thus it is considered a solar analog. The luminosity class 'V' means this is a main sequence star that is generating energy through the thermonuclear fusion of hydrogen at its core. The effective temperature of the outer envelope of HD 44594 is 5,840 K, which is giving it the characteristic yellow hue of a G-type star.This star has about 108% of the Sun's mass and is about the same radius as the Sun. It may be slightly younger than the Sun with an estimated age of 4.1 billion years. the abundance of elements other than hydrogen or helium, what astronomers term the star's metallicity, is 41% higher than in the Sun. The projected rotational velocity of the star is 4.4 km s−1, which gives the minimum azimuthal velocity along the star's equator.This star has been examined in the infrared using the Spitzer Space Telescope. However, no excess emission was discovered, which might otherwise have indicated the presence of a circumstellar debris disk of orbiting dust.

HD 38529d

HD 37974 (or R 126) a variable B[e] hypergiant in the Large Magellanic Cloud. It is surrounded by an unexpected dust disk.

LTT+2380
day

M1III

+33° 55′ 02.8577″

HD 44219 b is an extrasolar planet which orbits the G-type main sequence star HD 44219, located approximately 164 light years away in the constellation Monoceros. This planet has at least three-fifths the mass of Jupiter and takes 1.29 years to orbit the star at a semimajor axis of 1.18 AU. However unlike most other known exoplanets, its eccentricity is not known, but it is typical that its inclination is not known. This planet was detected by HARPS on October 19, 2009, together with 29 other planets.

HD 40307 c is an extrasolar planet orbiting the star HD 40307, located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the HARPS apparatus, in June 2008. Of the six proposed planets in the HD 40307 star system, it is the third-largest, and has the second-closest orbit from the star. The planet is of interest as this star has relatively low metallicity, supporting a hypothesis that different metallicities in protostars determine what kind of planets they will form.

Lick and Keck Observatory

HD 40307 b is an extrasolar planet orbiting the star HD 40307, located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Obervatory's HARPS apparatus, in June 2008. It is the second smallest of the planets orbiting the star, after HD 40307 e. The planet is of interest as this star has relatively low metallicity, supporting a hypothesis that different metallicities in protostars determine what kind of planets they will form.

HD 3883

HD 42818 (HR 2209) is a star in the constellation Camelopardalis.HD 42818 is a white A-type main sequence dwarf with an apparent magnitude of +4.76. It is approximately 176 light years from Earth.

G0IV

Fischer et al.

HD 40873 is a star in the northern constellation of Auriga. Located around 440 light-years distant, it shines with a luminosity approximately 38 times that of the Sun and has a surface temperature of 7,753 K. It is a suspected variable star.Samuel Molyneux named this star Telescopica in Auriga. Flamsteed catalogued it as 35 Camelopardali Heveliana, which is the name James Bradley continued to use, although it is within the borders of the modern constellation Auriga.

HD 4113

HD 40307 c is an extrasolar planet orbiting the star HD 40307, located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the HARPS apparatus, in June 2008. Of the six proposed planets in the HD 40307 star system, it is the third-largest, and has the second-closest orbit from the star.

HD 4391 is a triple star system in the constellation Phoenix that is located at a distance of 48.7 light years from the Sun. The primary has a stellar classification of G3V, which is a G-type main sequence star. The physical properties of this star are similar to the Sun, making it a solar analog. However, it is believed to have 22% greater mass than the Sun and is only 1.2 billion years old. The spectrum for this star displays an abnormally low level of beryllium, which may be the result of some form of mixing process.No planet has been detected in orbit around this star, nor does it emit a statistically significant excess of infrared radiation that might indicate a debris disk. However, it has two companions that share a common proper motion through space with HD 4391, effectively making it a triple star system. The first, a red dwarf of type M4, lies at an angular separation of 17″ from the primary. The second is a type M5 star at a separation of 49″.
G3V

−0.13

HD 44219b

HD 40307 e is an extrasolar planet orbiting the star HD 40307. It is located 42 light-years away in the direction of the southern constellation Pictor.

G1V

HD 43691b

HD 4203 b

F8V

suspected

HD 41004 B

A7 V

HD 37605 b is an extrasolar planet that has nearly three times more mass than Jupiter. It orbits close to the star, taking 54 days to revolve around the parent star HD 37605. Its orbit is highly eccentric, around 74%.

G5 IV

HD 45350b

HD 41004 A

G8V

HD 4208

HD 40979A

HD 44219 b is an extrasolar planet which orbits the G-type main sequence star HD 44219, located approximately 164 light years away in the constellation Monoceros. This planet has at least three-fifths the mass of Jupiter and takes 1.29 years to orbit the star at a semimajor axis of 1.18 AU. However unlike most other known exoplanets, its eccentricity is not known, but it is typical that its inclination is not known.

Cochran et al.

HD 4313b

HD4308

HD 38283b

HR 2209

HD 38529 Ac

HD 4335

HD 37124b

F6V/K-MV

HIP+3391

Oct 26, 2007

HD 41004 A b

HD 40307d

B8IV + B9.5V

HD 40307 b is an extrasolar planet orbiting the star HD 40307, located 42 light-years away in the direction of the southern constellation Pictor. The planet was discovered by the radial velocity method, using the European Southern Obervatory's HARPS apparatus, in June 2008. It is the second smallest of the planets orbiting the star, after HD 40307 e.

HD 37605 b