104 Tauri

{{Starbox begin

| name = 104 Tauri

}}

{{Starbox observe

| epoch = J2000

| constell = Taurus

| ra = {{RA|05|07|27.00529}}

| dec = {{DEC|+18|38|42.1815}}

| appmag_v = 4.92

}}

{{Starbox character

| class = G4V

| b-v = 0.64

| u-b =

| variable =

}}

{{Starbox astrometry

| radial_v = +20.19

| prop_mo_ra = +534.73

| prop_mo_dec = +17.93

| parallax = 64.79

| p_error = 0.33

| parallax_footnote =

| absmag_v = {{Val|3.75|0.06}}

}}

{{Starbox detail

| mass = {{Val|1.00|0.03|0.04}}

| radius = {{Val|1.63|0.06}}

| gravity = 4.06

| metal_fe = −0.22

| temperature = 5,717

| luminosity = 2.41

| rotational_velocity = 10.00

| rotation =

| age_gyr = 10.15

}}

{{Starbox catalog

| names = m Tau, 104 Tau, BD+18°779, GJ 188, HD 32923, HIP 23835, HR 1656, SAO 94332

}}

{{Starbox reference

|Simbad=104+Tau

}}

104 Tauri (104 Tau) is the Flamsteed designation for a star in the equatorial constellation of Taurus. It has an apparent magnitude of 4.92, which is bright enough to be seen with the naked eye. Based upon parallax measurements, this star is located about 50 light-years from the Sun. It is moving further from the Sun with a heliocentric radial velocity of +20 km/s.

This star has a stellar classification of G4 V, which suggests it is an ordinary G-type main-sequence star that is generating energy through hydrogen fusion at its stellar core. It is an estimated 10 billion years old and is spinning with a projected rotational velocity of 10 km/s. The star has about the same mass as the Sun, with 1.6 times the Sun's radius. It is radiating 2.4 times the Sun's luminosity from its photosphere at an effective temperature of {{val|5717|ul=K|fmt=commas}}.

104 Tauri appears to have a modest barium enrichment compared to iron. This may indicate that the star had accreted stellar wind of a companion star in the asymptotic giant branch, which has since evolved into a white dwarf.

The star displays convincing evidence for an infrared excess, suggesting the presence of a circumstellar debris disk of dust.

On 24 July 2028, it will be occulted by Venus over Japan, East Siberia and the Pacific Ocean.{{cite book |date=2002 |first=Jan |last=Meeus |chapter=Mutual occultations of planets |pages=174–185 |title=More Mathematical Astronomy Morsels |isbn=0943396743 |url=https://falakmu.id/khgt/dokumen/More%20mathematical%20astronomy%20morsels%20(Jean%20Meeus)%20(Z-Library).pdf}}{{rp|165}}

References

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{{citation

| title=m Tau -- Double or multiple star

| work=SIMBAD Astronomical Database

| publisher=Centre de Données astronomiques de Strasbourg

| url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=104+Tauri

| accessdate=2013-08-12

| postscript=.

}}

{{cite journal

| title=The barium-to-iron enrichment versus age relation of ancient disc stars

| journal=Monthly Notices of the Royal Astronomical Society

| publisher=Oxford University Press (OUP)

| volume=471 | issue=3 | pages=3768–3774

| date=2017-07-21

| bibcode=2017MNRAS.471.3768F

| doi=10.1093/mnras/stx1848

| doi-access=free | issn=0035-8711

}}

Category:Taurus (constellation)

Category:G-type main-sequence stars

Category:Double stars