Alsafi - σ Draconis (sigma Draconis)
Alsafi, also designated as σ Draconis (sigma Draconis), is a variable hypergiant star in the constellation of Draco.
Alsafi visual magnitude is 4.68. Because of its moderate brightness, Alsafi should be easily visible from locations with dark skyes, while it can be barely visible, or not visible at all, from skyes affected by light pollution.
The table below summarizes the key facts about Alsafi:
Alsafi - σ Draconis (sigma Draconis) is above the horizon from Greenwich, United Kingdom .
Altitude: 57.5°
Azimuth: 326.1°
Direction: North-West
Celestial coordinates and finder chart of Alsafi
Alsafi is situated close to the northern celestial pole and, as such, it is visible for most part of the year from the northern hemisphere. Celestial coordinates for the J2000 equinox as well as galactic coordinates of Alsafi are provided in the following table:
The simplified sky map below shows the position of Alsafi in the sky:

Visibility of Alsafi from your location
Location: Greenwich, United Kingdom
Latitude: 51° 28’ 47” N
Longitude: 0° 00’ 00” E
Timezone: Europe/London
Alsafi - σ Draconis (sigma Draconis) is circumpolar and transits at 14:24 UTC (altitude: 71.8°)
Digitized Sky Survey image of Alsafi
The image below is a photograph of Alsafi from the Digitized Sky Survey 2 (DSS2 - see the credits section) taken in the red channel. The area of sky represented in the image is 0.5x0.5 degrees (30x30 arcmins). The proper motion of Alsafi is 0.6 arcsec per year in Right Ascension and -1.738 arcsec per year in Declination and the associated displacement for the next 100 years is represented with the red arrow.

Distance of Alsafi from the Sun and relative movement
Alsafi is distant 18.80 light years from the Sun and it is moving far from the Sun at the speed of 27 kilometers per second.
Spectral properties of Alsafi
Alsafi belongs to spectral class K0 and has a luminosity class of V corresponding to a hypergiant star.
The red dot in the diagram below shows where Alsafi is situated in the Hertzsprung–Russell diagram.
