M67
Messier 67 (also known as M67 or NGC 2682) is an open cluster in the constellation of Cancer. M67's Trumpler class is variously given as II 2 r, II 2 m, or II
3 r. It was discovered by Johann Gottfried Koehler in 1779. Age estimates for the cluster range between 3.2 and 5 billion years, with the most recent estimate (4 Gyr) implying stars in M67 are younger than the Sun. Distance estimates are likewise varied and typically range between 800–900 pc. Recent estimates of 855, 840, and 815 pc were established via binary star modelling and infrared colour-magnitude diagram fitting, accordingly.
M67 is not the oldest known open cluster, but Galactic clusters known to be older are few, and none of those is closer than M67. The latter is an important laboratory for studying stellar evolution, since the cluster is well populated, negligible amounts of dust obscuration, and all its stars are at the same distance and age, except for approximately 30 anomalous blue stragglers, whose origins are not fully understood.
This artist’s impression video shows a hot Jupiter exoplanet orbiting close to a star in Messier 67.
M67 is probably the second best observed open cluster after the Hyades cluster, which is amongst the nearest open clusters and younger than M67. M67 is one of the most-studied open clusters, yet estimates of its physical parameters such as age, mass, and number of stars of a given type, vary substantially. Richer et al. estimate its age to be 4 billion years, its mass to be 1080 solar masses, and the number of white dwarfs to be 150. Hurley et al. estimate its current mass to be 1400 solar masses and its initial mass to be approximately 10 times as great.
M67 has more than 100 stars similar to the Sun, and numerous red giants. The total star count has been estimated at well over 500. The ages and prevalence of Sun-like stars contained within the cluster had led astronomers to consider M67 as the possible parent cluster of the Sun. However, computer simulations have suggested that this is highly unlikely to be the case.
The cluster contains no main sequence stars bluer than spectral type F, other than perhaps some of the blue stragglers, since the brighter stars of that age have already left the main sequence. In fact, when the stars of the cluster are plotted on the Hertzsprung-Russell diagram, there is a distinct "turn-off" representing the stars which have terminated hydrogen fusion in the core and are destined to become red giants. As the cluster ages, the turn-off moves progressively down the main sequence.
It appears that M67 does not contain an unbiased sample of stars. One cause of this is mass segregation, the process by which lighter stars (actually, systems) gain speed at the expense of more massive stars during close encounters, which causes the lighter stars to be at a greater average distance from the center of the cluster or to escape altogether
A March 2016 joint AIP/JHU study by Barnes at al. on rotational periods of 20 Sun-like stars, measured by the effects of moving starspots on light curves, suggests that these approximately 4 Gyr old stars spin for about 26 days - much like our Sun, which has a period at the equator of 25.38 days. Measurements were carried out as part of the extended K2 mission of Kepler space telescope. This discovery strengthens the solar-stellar connection, a fundamental principle of modern solar and Stellar astrophysics. Sydney Barnes (first author of the study) commented: "We had predicted this would occur, but it has been a real privilege to have been able to actually make the measurements." Co-author Jörg Weingrill adds: "With the measured rotational periods for stars up to the age of our Sun we can now confidently trace back the evolution of our home star."
