HIP 78530 b

Last updated
HIP 78530 b
Discovery
Discovered by David Lafrenière et al. [1]
Discovery site Gemini Observatory North, Flag of the United States.svg  USA [1]
Discovery datePublished January 24, 2011 [2]
Direct imaging [1]
Orbital characteristics
Epoch J2000
710 (± 60) [3] AU
~12000 [1] y
Star HIP 78530
Physical characteristics
1.83±0.16  RJ [4]
Mass 23.04 (± 4) [3] MJ
Temperature 2800 (± 200) [1]

    HIP 78530 b is an object that is either a planet or a brown dwarf in the orbit of the star HIP 78530. It was observed as early as 2000, but the object was not confirmed as one in orbit of the star HIP 78530 until a direct imaging project photographed the star in 2008. The image caught the attention of the project's science team, so the team followed up on its initial observations. HIP 78530 b orbits a young, hot, bright blue star in the Upper Scorpius association. The planet itself is over twenty-three times more massive than Jupiter, orbiting eighteen times further from its host star than Pluto does from the Sun by the estimates published in its discovery paper. In this predicted orbit, HIP 78530 b completes an orbit every twelve thousand years. [1]

    Contents

    Discovery

    Between 2000 and 2001, the ADONIS system at the ESO 3.6 m Telescope in Chile detected a faint object in the vicinity of HIP 78530. This object was reported in 2005 and 2007, although the astronomers investigating the star were not able to tell, based on their observations, if the faint object was an orbiting companion or not. The team did not follow up on this. [1]

    The North telescope of the Gemini Observatory, which directly imaged the HIP 78530 system. Gemini Observatory at sunset.jpg
    The North telescope of the Gemini Observatory, which directly imaged the HIP 78530 system.

    The random selection of ninety-one stars in the Upper Scorpius association provided a sample of stars to be observed using the Near Infrared Imager and Spectrometer (NIRI) and Altitude conjugate Adaptive Optics for the Infrared (ALTAIR) adaptive optics system at the Gemini Observatory. Among the ninety stars selected for direct imaging was the star HIP 78530, which was first imaged by the camera on May 24, 2008. [1] This initial image revealed the presence of the same faint object within the vicinity of HIP 78530. [1]

    Follow-up imaging took place on July 2, 2009, and August 30, 2010, using the same instruments, as astronomers hoped to reveal this companion object's proper motion, or the rate that it moves over time. Additional follow-up data was recovered in the spring and summer of 2010, but large errors in the data's astrometry led the investigating astronomers to disregard it. The observations over the three years was compiled, with the data used to filter out pixelated portions of the images and improve the images' quality. The result suggested not only that the faint object in the image was nearby the star HIP 78530, but that it was a brown dwarf or planet in size. Further study would be needed to prove its true nature. [1]

    On July 2, 2009, July 3, 2009, and August 8, 2009, use of the NIFS integral field spectrograph with ALTAIR allowed the astronomers to collect data on the spectrum of the faint object and its star. Analysis of the spectra and the objects' astrometry (how the star and the faint object change position in the sky) led to the confirmation of the companion HIP 78530 b. [1]

    The confirmation of HIP 78530 b was reported on January 24, 2011. [2] In imaging the ninety-one stars, HIP 78530 b and 1RXSJ1609-2105b were discovered. [1] The discoveries of these two orbiting bodies allowed astronomers to predict that bodies with such low planet/brown dwarf-to-star mass ratios (below 0.01) orbiting at a distance of hundreds of AU exists in the orbits of 2.2+5.5
    −1.9    % of all stars. [1] However, this number is a lower limit, as astronomers have been unable to detect smaller, low-mass planets that fit this scenario.

    Host star

    HIP 78530
    Observation data
    Epoch J2000       Equinox J2000
    Constellation Scorpius
    Right ascension 16h 01m 55.44s
    Declination −21° 58′ 49.77″
    Apparent magnitude  (V)7.1691±0.0459
    Characteristics
    Spectral type B9V
    Astrometry
    Proper motion (μ)RA: −12.0126±0.123948  mas/yr [5]
    Dec.: −24.1124±0.0703451  mas/yr [5]
    Parallax (π)7.28477 ± 0.078398  mas [5]
    Distance 445.8+4.87
    −4.77      ly
    (136.759+1.493
    −1.462      pc) [5]
    Details [5]
    Mass 2.192+0.45
    −0.24      M☉
    Radius 2.109+0.067
    −0.059      R☉
    Luminosity 23.36  L☉
    Surface gravity (log g)4.68+0.02
    −0.01      cgs
    Temperature 10690+24
    −10      K
    Metallicity [Fe/H]−0.5+0.03
    −0.01      dex
    Age 5  Myr
    Database references
    SIMBAD data

    HIP 78530 is a luminous, blue B-type main sequence star in the Upper Scorpius association, a loose star cluster composed of stars with a common origin. [1] The star is estimated to be approximately 2.2 times the mass of the Sun. [5] Ages of the Upper Scorpius group have been quoted at 5 million years, however a more recent estimate suggests that the group is somewhat older (approximately 11 million years old). [6] Its effective temperature is estimated at 10500 K, [3] less than twice the effective temperature of the Sun. [7]

    HIP 78530 has an apparent magnitude of 7.18. [3] It is incredibly faint, if visible at all, as seen from the unaided eye of an observer on Earth. [8]

    Characteristics

    HIP 78530 b is most likely a brown dwarf, a massive object that is large enough to fuse deuterium (something that planets are too small to do) but not large enough to ignite and become a star. Because HIP 78530 b's characteristics blend the line between whether or not it is a brown dwarf or a planet, astronomers have tried to determine what HIP 78530 b is by predicting whether it was created in a planet-like or star-like (how brown dwarves are formed) manner. [1]

    Its estimated mass is over 23.04 times that of Jupiter. Additionally, HIP 78530 b orbits its host star at an estimated average distance of 710 AU, [3] which is 710 times the average distance between the Earth and the Sun assuming the brown dwarf has a circular orbit. [1] The average distance between dwarf planet Pluto and the Sun is 39.482 AU, meaning that HIP 78530 b orbits its host star nearly eighteen times further than Pluto orbits the Sun. [9] In accordance with the data, HIP 78530 b would complete an orbit approximately every 12,000 years, although the actual orbital motion of HIP 78530 b is most likely smaller than 710 AU, but it has not been directly observed long enough to know definitively. [1]

    Related Research Articles

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    References

    1. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 Lafrenière, D.; Jayawardhana, R. (2011). "DISCOVERY OF A ~23 MJup BROWN DWARF ORBITING ~700 AU FROM THE MASSIVE STAR HIP 78530 IN UPPER SCORPIUS". Astrophysical Journal . 730 (1): 42. arXiv: 1101.4666 . Bibcode:2011ApJ...730...42L. doi:10.1088/0004-637x/730/1/42. S2CID   119113383.
    2. 1 2 David Lafrenière; Ray Jayawardhana; Markus Janson; Christiane Helling; Soeren Witte; Peter Hauschildt (2011). "Discovery of a ~23 Mjup Brown Dwarf Orbiting ~700 AU from the Massive Star HIP 78530 in Upper Scorpius". The Astrophysical Journal. 730 (1): 42. arXiv: 1101.4666 . Bibcode:2011ApJ...730...42L. doi:10.1088/0004-637X/730/1/42. S2CID   119113383.
    3. 1 2 3 4 5 Jean Schneider. "Notes for star HIP 78530". Extrasolar Planets Encyclopaedia . Archived from the original on May 5, 2011. Retrieved 10 June 2011.
    4. ↑ Pecaut, Mark J.; Mamajek, Eric E.; Bubar, Eric J. (2012-02-20). "A Revised Age for Upper Scorpius and The Star-Formation History Among the F-Type Members of the Scorpius-Centaurus OB Association". The Astrophysical Journal. 746 (2): 154. arXiv: 1112.1695 . doi: 10.1088/0004-637X/746/2/154 . ISSN   0004-637X.
    5. 1 2 3 4 5 6 "HIP 78530 Overview". NASA Exoplanet Archive. Retrieved December 20, 2023.
    6. ↑ Mark J. Pecaut; Eric E. Mamajek; Eric J. Bubar (February 2012). "A Revised Age for Upper Scorpius and the Star Formation History among the F-type Members of the Scorpius-Centaurus OB Association". Astrophysical Journal. 746 (2): 154. arXiv: 1112.1695 . Bibcode:2012ApJ...746..154P. doi:10.1088/0004-637X/746/2/154. S2CID   118461108.
    7. ↑ "Kepler Discoveries". Ames Research Center . NASA. 2011. Archived from the original on 2010-05-27. Retrieved 10 June 2011.
    8. ↑ "Stellar Magnitudes". Physics and Astronomy Department. University of Tennessee, Knoxville. Retrieved 10 June 2011.
    9. ↑ David Williams (2010). "Pluto Fact Sheet". Goddard Space Flight Center . NASA . Retrieved 10 June 2011.

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