Water vapour masers in long-period variable stars - III. Mira variables U Her and RR Aql

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Table 5

H₂O maser luminosities, stellar luminosities, and mass-loss rates of the semiregular variable stars from Paper I and II and the Mira variables U Her and RR Aql.

Star	Type	D	$\log L_{H_{2} O}^{up}$ $\log L_{{{\rm{H}}_2}{\rm{O}}}^{{\rm{up}}}$	log S (tot) ,log L_p						log L_bol	logṀ
		[pc]	[L_⊙]	[Jy km s⁻¹] , [s⁻¹]						[L_⊙]	[M_⊙ yr⁻¹]

				High		Mean		Low
R Crt	SRV	236	−4.88	3.5	44.0	2.9	43.4	2.3	42.8	4.03 ± 0.10	−5.46
RT Vir	SRV	226	−5.16	3.3	43.8	2.8	43.3	2.3	42.8	3.70 ± 0.09	−6.05
RX Boo	SRV	136	−6.23	2.6	42.7	1.9	41.9	1.5	41.5	3.58 ± 0.11	−6.12
SV Peg	SRV	333	−6.42	1.6	42.4	0.9	41.7	<0.8	<41.6	3.93 ± 0.20	−6.04
U Her	Mira	266	−5.77	2.6	43.3	2.0	42.6	1.5	42.1	3.71 ± 0.17	−6.25
RR Aql	Mira	410	−5.37	2.7	43.7	2.1	43.1	1.4	42.4	3.75 ± 0.15	−5.84

Notes. Column ‘D’ lists distances as given in Table 1, Papers I and II. Characteristic levels of H₂O maser brightness (S (tot) = integrated flux densities) and maser luminosities $(L_{H_{2} O}^{up} [L_{⊙}]; L_{p} [{photons s}^{- 1}])$ $\left( {L_{{{\rm{H}}_2}{\rm{O}}}^{{\rm{up}}}\left[ {{L_ \odot }} \right];{L_{\rm{p}}}\left[ {{\rm{ photons }}{{\rm{s}}^{ - 1}}} \right]} \right)$ are listed for the time range 1987–2015 for all sources except RX Boo and SV Peg (1987–2005; cf. Paper I). The definition of the levels (High, Mean, Low) is described in the text. Columns log L_bol and log Ṁ list stellar luminosities and mass-loss rates.

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