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A Herbig AeBe star is an A-type star or B-type star with Balmer series emission lines and with excess infrared due to surrounding dust. The term is presumably used referring to a set of such stars, a specific star being generally called a Herbig Ae star (HAe) or a Herbig Be star (HBe), according to its spectral class. Their luminosity is high for their spectral class. They were first described by George Herbig in 1960. Many are highly variable, and many have calcium emission lines. They are considered to be pre-main-sequence stars (PMSs) more massive than T-Tauri stars (TTSs), i.e., 2 solar masses or more, but a PMS above about 8 solar masses would reach the main sequence so quickly that such detection is highly unlikely.
Note that Be stars have the same spectral classes and have Balmer emission lines, but their characteristics are due to rapid rotation and they are not PMSs.