The detached dust shells around the carbon AGB stars R Sculptoris and V644 Scorpii

M. Maercker; S. Ramstedt; M. L. Leal-Ferreira; G. Olofsson; H. G. Floren

doi:10.1051/0004-6361/201424892

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Volume 570 (October 2014)

A&A, 570 (2014) A101

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Table 2

Measured shell radii (R) and shell widths (ΔR – FWHM of Gaussian distribution) for R Scl and V644 Sco.

	R Scl		V644 Sco
	R[′′]	ΔR[′′]	R[′′]	ΔR[′′]

this paper	19.7	3.2	9.4	2.0
GD2001^a	20.7	–	–	–
GD2003^b	20.0	2.0	–	–
S2005 (dust)^c	27.0	–	17.0	–
S2005 (gas)^c	20.1	–	10.5	–
O2010^d	19.2	1.2	–	–
M2012^e	18.5	1.3	–	–

Notes. Both can be determined to with ±0.̋5. The results from this paper are derived from radiative transfer models constrained by the polarised intensity images from PolCor (see Fig. 5). The results are compared to previous estimates of the detached shells. resonance lines; .

^(a)

Based on observations stellar light scattered in NaD and K;

^(b)

based on polarised, dust-scattered stellar light;

^(c)

based on dust and gas radiative transfer models;

^(d)

based on observations of dust scattered stellar light;

^(e)

based on fit to observed CO(3−2) line emission with ALMA

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