Celestial hemisphere:  Southern  ·  Constellation: Ophiuchus (Oph)  ·  Contains:  HD152997  ·  HD153240  ·  M 10  ·  NGC 6254  ·  PGC 1059966  ·  PGC 1067786
Getting plate-solving status, please wait...
M10 Globular Cluster in Ophiucus, Mau_Bard
M10 Globular Cluster in Ophiucus, Mau_Bard

M10 Globular Cluster in Ophiucus

Revision title: Wide Field

Getting plate-solving status, please wait...
M10 Globular Cluster in Ophiucus, Mau_Bard
M10 Globular Cluster in Ophiucus, Mau_Bard

M10 Globular Cluster in Ophiucus

Revision title: Wide Field

Equipment

Loading...

Acquisition details

Loading...

Description

M10

M10 (also designated NGC 6254) is a globular cluster discovered by Charles Messier in 1764, who described it as a "nebula without stars".  Using larger instrumentation, William Herschel was able to resolve the cluster into its individual star members. The first to estimate the distance to the cluster was Harlow Shapley, although his derivation of 33 kly was much further than the modern value of 14.3 kly.

Its galactic coordinates are (15°, 24,2°), that means it is above the galactic plane. The cluster is currently located about 16 kly from the Galactic Center.
It completes an orbit around the Milky Way galaxy about every 140 million years, during which it crosses the plane of the galactic disk.

The tidal radius (*) of M10 is 19.3 arcminutes, which is about two-thirds of the apparent diameter of the Moon. M10 has a spatial diameter of 83 light-years.

Messier 10 is "moderately metal–poor". The abundance of iron, measured as [Fe/H] equals –1.45 ± 0.04 dex, is only 3.5% of the abundance found at the surface of the Sun.

Because binary stars are, on average, more massive than normal stars, the binaries tend to migrate toward the center of the cluster. The fraction of binary stars in the core region is about 14%. This proportion decreases with increasing radius to about 1.5% in the outlying regions of the cluster. Correspondingly, the core region contains a concentration of interaction-formed blue straggler stars, most of which formed 2–5 billion years ago. The density of stars in the core region is about 3.8 solar masses per cubic parsec.

Other data:
Mass 2.25 × 10^5 M☉
Estimated age 11.39 Billion Years (Gy)

(*) The tidal radius is the distance from the center of the globular cluster at which the external gravitation of the galaxy has more influence over the stars in the cluster than does the cluster itself.

Comments