Microturbulence across the Hertzsprung–Russell Diagram - Setting observational constraints on Milky Way stars

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Volume 701 (September 2025)

A&A, 701 (2025) A297

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Table 3

Micro-turbulence and the deficit of slow rotators for Galactic stars of various parameters separated by spectral type (OBAFGK), luminosity class (dw – dwarfs; g – giants; sg – supergiants) and initial stellar mass: Group 1 – M_init ≳15 M_⊙; Group 2 – 8 M_⊙ ≲M_init ≲15 M_⊙; Group 3 – 3 M_⊙ ≲M_init ≲8 M_⊙; Group 4 – 3 M_⊙ ≲M_init ≲1 M_⊙.

Parameter	Group 1									Group 2			Group 3			Group 4
	O dw		O g/sg			B g/sg		A	F	B		AFG	B		FG	AF	GK
in km s⁻¹	Hot	Cool	Hot	Cool	Hot	Inter	Cool	sg	sg	dw	g/sg	g/sg	dw	g	g	dw	dw
${\bar{v}}_{mic}$ $\[\bar{v}_{\text {mic}}\]$	...	8^a	...	18^a	18^a	15/20^a	7.4(1.8)	7.0(1.8)	4.3(1.1)	3.8(3.3)	...	4.5/3.9/3.2	2.1(2.2)	3.8(1.6)^b	3.2(0.9)	3.0(2.4)	0.8(0.1)
$\bar{vsini (upl)}$ $\[\overline{\text { vsini (upl)}}\]$	60	10	65	30	30	25/30	15	≲5	≲5	≲5	20	≲5	≲5	12	≲5	9	≲2

Notes. ${\bar{v}}_{mic}$ $\[\bar{v}_{\text {mic}}\]$ − mean value of v_mic averaged over the corresponding mass and temperature regime and its standard error (in brackets); $\bar{vsini (upl)}$ $\[\overline{\text { vsini (upl)}}\]$ – a “by eye” average over nearby stars of similar upper detectability limit to v sin i; “a” – a “by eye” estimate; “b” – an estimate corresponding to the sample SPBs.

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