An Etymological Dictionary of Astronomy and Astrophysics
English-French-Persian

1) (Adj.) Being or acting at the middle place or stage, or between extremes.
2a) (n.) A person who acts between others; something intermediate.
2b) Chemistry: A molecular entity that is formed (directly or indirectly) from the reactants and reacts further to give (either directly or indirectly) the products of a chemical reaction (PAC, 1996, 68, 149, A glossary of terms used in chemical kinetics, including reaction dynamics, IUPAC Recommendations 1996).
See also:
→ intermediate boson, → intermediate frequency, → intermediate infrared, → intermediate-mass black hole, → intermediate-mass protostar, → intermediate-mass star.

Intermediate, from M.L. intermediatus "lying between," from L. intermedius "that which is between," from → inter- "between" + medius "located in the middle;" PIE root *medhyo- "middle;" cf. Pers. miyân, as below; Av. maidiia-, Skt. mádhya-; Gk. medos, messos "middle;"

Miyâni, adj. of miyân "within, between, center," from Mid.Pers. mayân "middle; among, between," Av. maidiia- "middle, the middle," maiδiiāna- "middle, center;" cf. Skt. mádhya- "middle, located in the middle;" G.H.G. mitti "located in the middle."
Andarmiyâni, adj. of andarmiyân "in the middle," from andar-, → inter-, + miyân, as above.
Miyânji "intermediary, mediator," from Mid.Pers. mayânjig, from mayân.

A hypothetical → elementary particle that mediates the → weak interaction, carrying its effect from one particle to another as the photon does for electromagnetic interactions. First introduced in 1961 by Sheldon Glashow.

→ intermediate; → boson.

In a → superheterodyne receiver, a frequency resulting from the combination of the received modulated → carrier frequency and the → local oscillator frequency.

→ intermediate; → frequency.

The infrared radiation with wavelengths between about 1.5 and 20 microns. → near infrared; → far infrared.

→ intermediate; → infrared.

A → black hole with a mass in the range 10²-10⁴ solar masses. IMBHs may form as the result of multiple → mergers of smaller objects in the centers of dense stellar clusters in the present universe, assuming → mass loss from → stellar winds is not significant. They may also arise from the evolution of → very massive stars early in the history of the Universe, forming black hole "seeds" in the centers of massive halos (the precursors of the galaxies we see today) early in the history of the Universe, to redshifts z > 10. Currently the best observational evidence for IMBHs comes from models of ultraluminous X-ray sources (See, e.g., J. M. Centrella et al. 2010, astro-ph/1010.5260).

→ intermediate; → mass; → black; → hole.

A protostar that evolves into an → intermediate-mass star.

→ intermediate; → mass; → protostar.

A star whose mass lies in the range about 2 to 8 → solar masses approximately.

→ intermediate; → mass; → star.