Milliarcsecond in the context of "HD 134060"

Beta Fornacis (Beta For, β Fornacis, β For) is solitary star in the southern constellation of Fornax. It is visible to the naked eye with an apparent visual magnitude of 4.46. Based upon an annual parallax shift of 18.46 mas, it is located around 177 light years away from the Sun. At that distance, the visual magnitude is reduced by an interstellar extinction factor of 0.1.

This is an evolved, G-type giant star with a stellar classification of G8 III. It is a red clump giant, which means it has undergone helium flash and is currently generating energy through the fusion of helium at its core. Beta Fornacis has 1.33 times the mass of the Sun and, at an age of 3.3 billion years, has expanded to 10.5 times the Sun's radius. It is radiating 51 times the solar luminosity from its outer atmosphere at an effective temperature of 4,790 K.

Delta Crateris (δ Crt, δ Crateris) is a solitary star in the southern constellation of Crater. With an apparent visual magnitude of 3.56, it is the brightest star in this rather dim constellation. It has an annual parallax shift of 17.017 mas as measured from Earth, indicating Delta Crateris lies at a distance of 192 ly from the Sun.

Beta Crateris, Latinized from β Crateris, is a binary star system in the southern constellation of Crater. It is visible to the naked eye with an apparent visual magnitude of 4.46. Based upon an annual parallax shift of 9.59 mas as seen from Earth, it is around 340 light years from the Sun.

This is an astrometric binary star system with an orbital period of 6.0 years and a projected separation of 8.3 AU. The orbit has an estimated semimajor axis of 9.3 AU. The primary component A is listed as an A-type giant star with a stellar classification of A2 III. However, Houk and Smith-Moore (1988) give a main sequence classification of A1 V, while Abt and Morrell (1995) list it as a subgiant star with a class of A2 IV. The spectrum shows enhanced barium, possibly as a result of a previous mass transfer event.

41 Arietis (abbreviated 41 Ari) is a triple star system in the northern constellation of Aries. With an apparent visual magnitude of 3.63, this system is readily visible to the naked eye. It has an annual parallax shift of 19.69 mas, which indicates it is at a distance of 166 light-years (51 parsecs) from the Sun.

The system consists of a binary pair, designated 41 Arietis A, together with a third companion star, 41 Arietis D. (41 Arietis B and C form optical pairs with A, but are not physically related.) The components of A are themselves designated 41 Arietis Aa (formally named Bharani /ˈbærəni/) and Ab.

R Doradus (HD 29712 or P Doradus) is a red giant variable star in the far-southern constellation Dorado, close to the border with Reticulum. Its distance from Earth is 178 light-years (55 parsecs). Having a uniform disk diameter of 57±5 mas, it is thought to be the extrasolar star with the largest apparent size as viewed from Earth.

Mu Serpentis, Latinized from μ Serpentis, is a binary star in the Serpens Caput (head) section of the equatorial constellation Serpens. It is visible to the naked eye with an apparent visual magnitude of 3.543. Based upon an annual parallax shift of 19.23 mas as seen from Earth, it is located around 170 light years from the Sun.

This is an astrometric binary for which coarse orbital elements have been determined based on interferometric observations. The pair orbit each other with a period of around 36 years and an eccentricity of roughly 0.4. The primary member, component A, is a white-hued A-type main sequence star with a stellar classification of A0 V. The nature of the secondary, component B, is less certain – it may be a class A or F type star of unknown luminosity class.

ν Serpentis, Latinized as Nu Serpentis, is a solitary star in the Serpens Cauda section of the equatorial constellation of Serpens. It is a white-hued star that is faintly visible to the naked eye with an apparent visual magnitude of 4.32. Based upon an annual parallax shift of 16.05 mas as seen from the Sun, it is about 203 light years from the Sun. The star is drifting further away with a radial velocity of +5 km/s.

This is an A-type main-sequence star with a stellar classification of A2V, and is generating energy through hydrogen fusion at its core. It is 350 million years old with a high rate of spin, showing a projected rotational velocity of 123 km/s. The star has 2.64 times the mass of the Sun and 3.0 times the Sun's radius. It is radiating 76 times the Sun's luminosity from its photosphere at an effective temperature of 9,120 K. Nu Serpentis has an optical companion, a magnitude +9.4 star at an angular separation of 46 arcseconds.

5 Vulpeculae is a single, white-hued star in the northern constellation of Vulpecula. It is situated amidst a random concentration of bright stars designated Collinder 399, or Brocchi's Cluster. This is a faint star that is just visible to the naked eye with an apparent visual magnitude of 5.60. Based upon an annual parallax shift of 13.8921±0.0900 mas, it is located around 235 light years from the Sun. It is moving closer with a heliocentric radial velocity of −21 km/s, and will make its closest approach in 2.5 million years at a separation of around 120 ly (36.89 pc).

This is a young A-type main-sequence star with a stellar classification of A0 V. It is a rapidly rotating star with a projected rotational velocity of 154 km/s. The star has an estimated 2.33 times the mass of the Sun and about 2.7 times the Sun's radius. It is radiating 34 times the Sun's luminosity from its photosphere at an effective temperature of 8,940 K.

2 Andromedae, abbreviated 2 And, is a binary star system in the northern constellation of Andromeda. 2 Andromedae is the Flamsteed designation. It is a faint star system but visible to the naked eye with a combined apparent visual magnitude of 5.09. Based upon an annual parallax shift of 7.7 mas, it is located 420 light years away. The binary nature of the star was discovered by American astronomer Sherburne Wesley Burnham at Lick Observatory in 1889. The pair orbit each other over a period of 74 years with a high eccentricity of 0.8.

The magnitude 5.26 primary, designated component A, is an A-type main-sequence star based on a stellar classification of A1V or A2V, although it may have already left the main sequence. It was identified as a candidate Lambda Boötis star, but this was ruled out by Paunzen et al. (2003) as it doesn't match the typical characteristics of these objects. Although 2 Andromedae does not display a significant infrared excess, it is a shell star that displays varying absorption features due to circumstellar dust grains. This may indicate it has an orbiting debris disk containing gas that is being viewed edge-on. The star is about 100 million years old and is spinning rapidly with a projected rotational velocity of 212 km/s.

Lambda Geminorum, Latinized from λ Geminorum, is a candidate multiple star system in the constellation Gemini. It is visible to the naked eye at night with a combined apparent visual magnitude of 3.57. The distance to this system is 101 light years based on parallax, and it is drifting closer with a radial velocity of –7.4 km/s. It is a member of what is suspected to be a trailing tidal tail of the Hyades Stream.

Components A and B of this system form a wide binary. The secondary, component B, is a magnitude 10.7 stellar companion at an angular separation of 9.29″ from the primary along a position angle of 35.72°, as of 2009. The primary was identified as a spectroscopic binary by E. B. Frost in 1924. This companion was confirmed during a lunar occultation with a separation of 14.1±0.7 mas and magnitude 6.8.

Phi Geminorum, Latinized from φ Geminorum, is a binary star in the constellation Gemini, to the southeast of Pollux. It is visible to the naked eye with an apparent visual magnitude of 4.95. Based upon an annual parallax shift of 14.66 mas, this system is located around 220 light years from the Sun.

The two components of this system have a circular orbit with a period of 582 days. The primary component is an A-type main sequence star with a stellar classification of A3 V. It is around 600 million years old and spinning relatively rapidly with a projected rotational velocity of 165 km/s. This rate of spin is giving the star an oblate shape with an equatorial bulge that is 6% larger than the polar radius. The star has nearly double the mass of the Sun and radiates 36.5 times the solar luminosity from its outer atmosphere at an effective temperature of 8,551 K.

35 Aquilae (abbreviated 35 Aql) is a star in the equatorial constellation of Aquila. 35 Aquilae is its Flamsteed designation though it also bears the Bayer designation c Aquilae. The apparent visual magnitude of this star is 5.8, which means it is a faint star but visible to the naked eye from dark suburban or rural skies. It has an annual parallax shift of 16.34 mas that is caused by the Earth's orbit around the Sun. This yields a distance estimate of 200 light-years (61 parsecs), give or take a 4 light-year margin of error. At this distance, the visual magnitude is diminished by 0.26 from extinction caused by interstellar gas and dust.

The spectrum of 35 Aquilae fits a stellar classification of A0 V, indicating it is an A-type main sequence star. Compared to the Sun, it has 210% of the mass and 180% of the radius. As such, it is much brighter than the Sun, emitting 14 times the luminosity from its outer atmosphere at an effective temperature of 8,939 K. This heat causes it to glow with the white-hot hue of an A-type star. 35 Aquilae is spinning rapidly with a projected rotational velocity of 110 km/s.

AX Circini is a binary star system in the southern constellation of Circinus. It has a nominal magnitude of 5.91, which is bright enough to be visible to the naked eye. Based upon an annual parallax shift of 1.7 mas, it is located roughly 1,900 light-years from the Earth. The system is moving closer with a heliocentric radial velocity of −21 km/s.

This is a spectroscopic binary with an orbital period of 17.88 years and an eccentricity of 0.19. A binary companion was first suspected in 1960, as the spectrum was considered to be composite and there is an ultraviolet excess. The companion was confirmed in 1982, and it was resolved using long baseline interferometry in 2014 and 2015. The system has an a sin i value of 6.05 AU, where a is the semimajor axis and i is the (unknown) orbital inclination.

Iota Cephei (ι Cephei, ι Cep) is a star in the northern constellation Cepheus. Based upon an annual parallax shift of 28.29 mas as seen from the Earth, it is located about 115 light years from the Sun. The star is visible to the naked eye with an apparent visual magnitude of 3.5.

It is a K-type giant star with a stellar classification of K0 III. It is currently at an evolutionary stage known as the red clump, indicating that it is generating energy through the fusion of helium at its core. It has 11 times the Sun's radius and about 2.15 times the mass of the Sun. Its luminosity is 57 times that of the Sun, and its surface has an effective temperature of 4,768 K.