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The data from Wallerstein (1962) is shown as red circles on top of the 2020 public data from the large scale stellar spectroscopic surveys APOGEE (DR16) and GALAH (DR3). The [α/Fe] versus [Fe/H] diagram refers to the graph, commonly used in stellar and galactic astrophysics. It shows the logarithmic ratio number densities of diagnostic ...
The galactic coordinate system is a celestial coordinate system in spherical coordinates, with the Sun as its center, the primary direction aligned with the approximate center of the Milky Way Galaxy, and the fundamental plane parallel to an approximation of the galactic plane but offset to its north. It uses the right-handed convention ...
Gaia Sky is an open-source astronomy visualisation desktop and VR program with versions for Windows, Linux and macOS.It is created and developed by Toni Sagristà Sellés in the framework of ESA's Gaia mission to create a billion-star multi-dimensional map of our Milky Way Galaxy, in the Gaia group of the Astronomisches Rechen-Institut (ZAH, Universität Heidelberg).
Galactic year. The galactic year, also known as a cosmic year, is the duration of time required for the Sun to orbit once around the center of the Milky Way Galaxy. [1] One galactic year is approximately 225 million Earth years. [2] The Solar System is traveling at an average speed of 230 km/s (828,000 km/h) or 143 mi/s (514,000 mph) within its ...
Helmi stream. The Helmi Stream is a stellar stream of the Milky Way galaxy. It started as a dwarf galaxy, now absorbed by the Milky Way as a stream. It was discovered in 1999, is formed of old stars deficient in heavy elements, and has a mass of 10 to 100 million solar masses. It was absorbed by the Milky Way some 6 to 9 billion years ago.
The locations within the Milky Way that have the highest stellar density are the central core and the interior of globular clusters. A typical mass density for a globular cluster is 70 M Sun pc −3 , which is 500 times the mass density near the Sun. [2] In the solar neighborhood, the stellar density of a star cluster must be greater than 0.08 ...
Initial mass function. The vertical axis is actually not ξ(m)Δm, but a scaled version of ξ(m). For m > 1 M ☉, it is (m/M ☉) −2.35. The mass of a star can only be directly determined by applying Kepler's third law to a binary star system. However, the number of binary systems that can be directly observed is low, thus not enough samples ...
Composite image showing young stars in and around molecular cloud Cepheus B.. This is a list of star-forming regions located in the Milky Way Galaxy and in the Local Group.Star formation occurs in molecular clouds which become unstable to gravitational collapse, and these complexes may contain clusters of young stars and regions of ionized gas called H II regions.