HD 113703

{{Starbox begin

| name = f Centauri

}}

{{Starbox observe

| epoch = J2000.0

| constell = Centaurus

| ra = {{RA|13|06|16.70}}

| dec = {{DEC|−48|27|47.8}}

| appmag_v = +4.71

}}

{{Starbox character

| type = Main sequence

| class = B4V + K0Ve

| b-v = {{val|−0.148|0.006}}

| u-b = −0.562

| variable =

}}

{{Starbox astrometry

| radial_v = {{val|+6.0|4.2}}

| prop_mo_ra = −29.558

| prop_mo_dec = −15.692

| parallax = 8.1592

| p_error = 0.1559

| parallax_footnote =

| absmag_v = −0.68

}}

{{Starbox detail

| source =

| component1 = f Cen Aa

| mass = 4.39

| radius =

| luminosity =

| temperature = 14,769

| gravity = 3.99

| metal_fe =

| age_myr = 92

| rotational_velocity = {{val|140|7}}

| component2 = f Cen C

| mass2 = 0.9

| temperature2 = 5,020

| luminosity2 = 0.49

| age_myr2 = 50

}}

{{Starbox catalog

| names = {{odlist | B=f Cen | HR=4940 | HD=113703 | CD=−47°8088 | HIP=63945 | SAO=223900 | GC=17750 | CCDM=J13063-4828 }}

}}

{{Starbox reference

| Simbad = HD+113703

}}

HD 113703, also known by the Bayer designation f Centauri, is a multiple star system in the southern constellation of Centaurus. The combined apparent visual magnitude of this system is +4.71, which is sufficient to make it faintly visible to the naked eye. The distance to this system is approximately 400 light years based on parallax measurements. It is a member of the Lower Centaurus Crux subgroup of the Scorpius–Centaurus association.

The primary of f Centauri is a blue-white hued B-type main-sequence star with a stellar classification of B4V. It is a young star with an age estimated at around 92 million years, and is spinning rapidly with a projected rotational velocity of 140 km/s. A close companion with a K magnitude of 9.16, designated component C, was detected in 2002 at an angular separation of {{val|1.55|ul=arcsecond}}. In 2013, a spectroscopic companion to the primary was observed using long baseline interferometry, with the two being designated components Aa and Ab.

A faint, magnitude 10.8 companion, component B, was first reported by J. F. W. Herschel in 1836. As of 2015, it was located at a separation of {{val|11.6|ul=arcsecond}} along a position angle of 78°. This is a K-type star with a class of K0Ve, showing emission in the Calcium H and K lines. It is a known BY Draconis variable star with the designation V1155 Centauri. It shares a common space motion with the primary, indicating a probable physical relationship, and its Gaia Data Release 3 parallax of {{val|7.965|0.018|ul="}} suggests a distance of 409 light years. The star shows a strong overabundance in lithium, which demonstrates its young age. It is about 0.8 magnitudes above zero age main sequence and thus is still contracting as a post-T Tauri star. X-ray emission has been detected from this star.

References

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}}

Category:B-type main-sequence stars

Category:K-type main-sequence stars

Category:Centaurus

Centauri, f

Category:Durchmusterung objects

113703

063945

4940

Category:Emission-line stars