Comparison of different populations of granular features in the solar photosphere

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Table 2

Properties of the umbral dots reported in the literature.

Ref.	Size	Continuum	Doppler	Magnetic field	Solar disk	Spatial	Method
	[arcsec]	intensity	velocity	strength [G]	position	resolution
		[I_c]	[km s^-1]		[arcsec]	[arcsec]

(1)	0.29–0.50	0.43–0.60	[−0.21, 0.12]	1400–2450	near	0.20	Individual features
					disk center
(2)	0.2	–	−1.0	–	disk center	0.13	Individual features
(3)	0.31	0.4–0.8	−0.8	–	(81, −296)	0.18	Multilevel tracking
							algorithm (MLT) of
							Bovelet & Wiehr (2001)
(4)	peak at 0.17	0.36–0.54	–	–	(−97, 81)	0.14	Low-noise curvature
							determination algorithm
							(Hamedivafa 2008)
(5)	0.29–0.35	0.25–0.69	[−0.6, 0.1]	1900–2700	(−131, −231)	0.32	MLT and curvature
							determination
							algorithm
(6)	0.4–0.57	0.23–0.26	–	–	–	–	MLT algorithm by
							Bovelet & Wiehr (2001)
(7)	–	–	[−1.4, 1.0]	–	(−382, −254)	0.14	Individual features
(8)	0.23–0.41	–	–	–	(−308, −564)	0.11	Crocker & Hoffman (2007)
							method
(9)	0.53–0.55	1.46–1.50	–	1000–2500	(385, −522)	0.13	Automatic detection
		I _ud / I _bg					algorithm by
							Bharti et al. (2010)
							and manual procedure
(10)	0.2–0.4	1.05–1.15	–	–	4 ARs	0.10	Identification
		I _ud / I _bg			around		and tracking method
					disk center		by Feng et al. (2014)

Reference. (1) Socas-Navarro et al. (2004); (2) Rimmele (2004); (3) Riethmüller et al. (2008); (4) Sobotka & Puschmann (2009); (5) Sobotka & Jurčák (2009); (6) Bharti et al. (2010); (7) Ortiz et al. (2010); (8) Kilcik et al. (2012); (9) Watanabe et al. (2012); (10) Ji et al. (2016).

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