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HD 984
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HD 984
HD 984 is a F-type main-sequence star located in the equatorial constellation Cetus. It is a young star, estimated 30 to 200 million years old, and is orbited by a brown dwarf companion. Parallax measurements by the Gaia spacecraft imply a distance of 150 light-years (46 pc) to HD 984. At an apparent magnitude of 7.32, the star is too dim to be visible to the naked eye.
The apparent magnitude of HD 984, i.e. its brightness relative to Earth, is 7.32. Such brightness is lower than the limit for naked-eye visibility, generally defined as 6.5m, meaning that HD 984 can't be seen with the naked eye. It may be visible by a small telescope or binoculars instead. The absolute magnitude, i.e. the magnitude of HD 984 if it was seen at 10 parsecs (32.6 ly), is 3.95. Kinematically, the system it is part of the Columba group. It has a relatively high proper motion.
The star is visually close (57") to BD-08 25, which is a star of apparent magnitude 9.14 unrelated to the system, being 1,800 light-years (550 pc) away from Earth based on its parallax. The galaxy NGC 47 lies just 320" from HD 984.
Based on the assumption that HD 984 is part of the Columba group, the stellar age would be of 30 Myr. However, there is still a possibility that HD 984 is a kinematic interloper or the Columba group is not sufficiently characterized to reliably assign an age. Previous isochronal ages of <0.48, 1.2+0.7
−0.9 and 3.1+1
−1.6 Gyr have been given by earlier studies. Since HD 984 A is a main sequence star, all isochronal ages will have high uncertainty.
An analysis by HD 984 B's discovery team say that the system is likely to be less than 200 million years, based on HD 984 A's rotation and stellar activity. The same research also says that ages less than 30 million years can be ruled out, based on isochronal age constraints for HD 984 B. Therefore, the age is very likely between 30 and 200 million years.
HD 984 A is a F-type main-sequence star, spectroscopically matching a class F7V. Those stars are typically larger, hotter and brighter than the Sun, and fuse hydrogen into helium at their core. HD 984 A is no expection, being 20% more massive than the Sun, 25% larger and over two times brighter. Its surface has an effective temperature of 6,326 K (6,053 °C), giving it a yello-white hue typical of F-type stars. HD 984 A rotates faster than 99% of all stars, with a rotation period estimated to be less than 1.6 days (38 hours). The Sun's rotational period is 27 days for comparison.
Its rotation, coronal activity and cromospheric activity indicates that it is a young and active main-sequence star, likely less than 200 million years old. It is expected to live 5 billion years on the main sequence. After that, it will cease its hydrogen at its core and evolve into a red giant star, increasing in size and luminosity, while decreasing in temperature.
HD 984 B is a brown dwarf, a class of astronomical objects that are intermediate between planets and stars, having masses between 13 and 75 MJ, and, unlike stars, can't produce thermonuclear fusion of hydrogen. It was discovered in 2015 by Meshkat et al., using direct imaging from the Apodizing Phase Plate coronagraph at the Very Large Telescope with NaCo.
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HD 984
HD 984 is a F-type main-sequence star located in the equatorial constellation Cetus. It is a young star, estimated 30 to 200 million years old, and is orbited by a brown dwarf companion. Parallax measurements by the Gaia spacecraft imply a distance of 150 light-years (46 pc) to HD 984. At an apparent magnitude of 7.32, the star is too dim to be visible to the naked eye.
The apparent magnitude of HD 984, i.e. its brightness relative to Earth, is 7.32. Such brightness is lower than the limit for naked-eye visibility, generally defined as 6.5m, meaning that HD 984 can't be seen with the naked eye. It may be visible by a small telescope or binoculars instead. The absolute magnitude, i.e. the magnitude of HD 984 if it was seen at 10 parsecs (32.6 ly), is 3.95. Kinematically, the system it is part of the Columba group. It has a relatively high proper motion.
The star is visually close (57") to BD-08 25, which is a star of apparent magnitude 9.14 unrelated to the system, being 1,800 light-years (550 pc) away from Earth based on its parallax. The galaxy NGC 47 lies just 320" from HD 984.
Based on the assumption that HD 984 is part of the Columba group, the stellar age would be of 30 Myr. However, there is still a possibility that HD 984 is a kinematic interloper or the Columba group is not sufficiently characterized to reliably assign an age. Previous isochronal ages of <0.48, 1.2+0.7
−0.9 and 3.1+1
−1.6 Gyr have been given by earlier studies. Since HD 984 A is a main sequence star, all isochronal ages will have high uncertainty.
An analysis by HD 984 B's discovery team say that the system is likely to be less than 200 million years, based on HD 984 A's rotation and stellar activity. The same research also says that ages less than 30 million years can be ruled out, based on isochronal age constraints for HD 984 B. Therefore, the age is very likely between 30 and 200 million years.
HD 984 A is a F-type main-sequence star, spectroscopically matching a class F7V. Those stars are typically larger, hotter and brighter than the Sun, and fuse hydrogen into helium at their core. HD 984 A is no expection, being 20% more massive than the Sun, 25% larger and over two times brighter. Its surface has an effective temperature of 6,326 K (6,053 °C), giving it a yello-white hue typical of F-type stars. HD 984 A rotates faster than 99% of all stars, with a rotation period estimated to be less than 1.6 days (38 hours). The Sun's rotational period is 27 days for comparison.
Its rotation, coronal activity and cromospheric activity indicates that it is a young and active main-sequence star, likely less than 200 million years old. It is expected to live 5 billion years on the main sequence. After that, it will cease its hydrogen at its core and evolve into a red giant star, increasing in size and luminosity, while decreasing in temperature.
HD 984 B is a brown dwarf, a class of astronomical objects that are intermediate between planets and stars, having masses between 13 and 75 MJ, and, unlike stars, can't produce thermonuclear fusion of hydrogen. It was discovered in 2015 by Meshkat et al., using direct imaging from the Apodizing Phase Plate coronagraph at the Very Large Telescope with NaCo.
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