What is Barnard's Star?

Barnard's Star (pronounced / brnrd /) is a very small red dwarf star, located near the -star Ophiuchus, on the northwest side of the 66-star Ophiuchus, only about 6 light away from the earth Years old. American astronomer Edward Emerson Barnard measured its self-property at 10.3 arc seconds per year in 1916, and is the star known to have the largest relative self-solarity. In honor of Barnard's discovery, the star was later called Barnard.

Barnard's Star (pronounced / brnrd /) is a very small mass
Barnard is a faint red dwarf of type M4 that observers must use a telescope to see. Its apparent magnitude is 9.54, compared with the brightest star Sirius (magnitude -1.5) and the darkest star (+6.0 magnitude) visible to the naked eye (the relationship of brightness is calculated on a logarithmic scale). The Barnard star at magnitude 9.54 is only 1 / 27th of the magnitude 6 magnitude.
Barnard is between 7 billion and 12 billion years old, and is not only older than the sun, but astronomers believe it may be the oldest star in the Milky Way. It has lost a large amount of rotational energy, and the cyclical changes in luminosity show that Barnard's star takes 130 days to complete a rotation (compared to 25 days for the sun) [1]
The Barnard star has become a hot planet that astronomers have noticed because it has several points of difference.
The first is autonomous speed
The second is close
The third and most attractive feature of Barnard is that there are likely to be two planets around this star about the size of Jupiter and Saturn orbiting it, another solar system close to us.
Because Barnard has several distinctive characteristics, it has become a star that attracts astronomers. Barnard is among all known stars
Generally speaking, stars are "constant and immobile" in our opinion, but in fact it is only because stars are usually hundreds, thousands or even tens of thousands of light years away from us, so even if there is motion, but due to their relative position The changes are small and hard to detect. However, if the stars are closer, it is relatively easy to see their changes. Astronomers call this phenomenon "the stars move on their own." But the star's own motion only reflects the tangential velocity of the star in the direction perpendicular to our line of sight. Stars are moving along the direction of our line of sight, and their velocity is called the apparent velocity.
In the 10 years since 1963, many astronomers have accepted Peter van der Verde's point of view: He claims to observe the perturbation of Barnard's self-movement, showing that it has one or more Big planet. Peter Vander has been observing this star since 1938, and
Astronomer Peter van de Kamp published an observation and analysis of Barnard's self-motion disturbance phenomenon in 1963, speculating that it may have a size approximately equal to Jupiter's
Barnard Star belongs to
The British Interplanetary Society revisited in the 1970s
constellation
Ophiuchus
Observers at 4 ° north latitude north of the equator can directly observe the Barnard star near the zenith. In theory, the Barnard star can be seen at 4 ° ± 90 ° north latitude, although close to the south Atmospheric extinction at the northern horizon will make the star's luminosity diminish, but it can still be seen at almost every latitude on Earth.
This star has many properties similar to the sun, and many of the stars adjacent to Barnard are the smallest and most common red dwarfs. The closest red dwarf currently to Barnard is Ross 154, with a distance of 5.41 light years (1.66 second gap). Relatively speaking, the sun and neighboring stars are the next closest galaxies to Barnard. [3] From the observation of the starry sky when standing on Barnard, the relative position of the sun on the celestial sphere is just east of the Unicorn, RA = 5 57 48.5, Dec = 04 ° 41 36 . Absolute star The Sun of magnitude 4.83 will be an impressive first-order star on the Barnard star with a gap of 1.834 seconds, similar to Beihe Three Phases for observers on Earth.

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