Abstract
Herbig Ae/Be stars are young contracting stars on the radiative track in the HR diagram on their way to the main sequence. These stars provide a valuable link between high and low mass stars. Here we review the progress that has been made in our understanding of these fascinating objects and their disks since the last major review on this topic published in 1998. We begin with a general overview of these stars and their properties. We then discuss the accretion of circumstellar material onto these stars. Next we discuss the dust and gas properties of the circumstellar disk before exploring the evidence for planet formation in these disks. We conclude with a brief discussion of future prospects for deepening our understanding of these sources and propose a new working definition of Herbig Ae/Be stars.
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Notes
This classification scheme should not be confused with the one proposed by Hillenbrand et al. (1992) where group I sources have an infrared excess that scales as \(\lambda ^{-4/3}\) longward of 2 μm, group II sources have an SED with a positive slope in the infrared, and group III sources have a minimal infrared excess.
However, experimental work by Gundlach et al. (2018) did not confirm the theoretical prediction that ices have higher tensile strengths than silicates.
GASPS (Gas Survey of Protoplanetary Systems has been an Open Time Herschel Key Program led by Bill Dent (Dent et al. 2013).
This method uses dust radial drift in a gas-rich disk to estimate gas masses. To first order, the spatial extent of the dust emission at different sub-mm wavelength is affected by the efficiency of dust drift and hence amount of gas in the disk; strictly, this works only for disks that do not show substructure.
This parameter depends on distance from the star \(r\) and is defined as \(Q(r)=c_{s}(r)\Omega /\pi G \Sigma _{g}(r)\), with \(c_{s}\) the sound speed, \(\Omega \) the angular velocity, \(G\) the gravitational constant and \(\Sigma _{g}\) the disks gas mass surface density.
Note that the term transitional disk is here reserved to disks that have no near-IR excess; HD 135344B and IRS 48 do have such an excess.
The surface density is here assumed as \(\Sigma (r) \propto r^{- \epsilon} \exp \left ( -\left (\frac{r}{R_{\text{tap}}} \right )^{2-\gamma} \right )\) with the radius \(r\) and the taper radius \(R_{\text{tap}}\).
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Funding
IK acknowledges funding from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). GM acknowledges funding from the Spanish project “On the Rocks II” (PGC2018-101950-B-100). RDO acknowledges funding for the STARRY project which received funding from the European Union’s Horizon 2020 research and innovation programme under MSCA ITN-EID grant agreement No 676036.
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Brittain, S.D., Kamp, I., Meeus, G. et al. Herbig Stars. Space Sci Rev 219, 7 (2023). https://doi.org/10.1007/s11214-023-00949-z
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DOI: https://doi.org/10.1007/s11214-023-00949-z