J/MNRAS/443/1629 Interferometry of chemically peculiar stars (Shulyak+, 2014)
Interferometry of chemically peculiar stars: theoretical predictions versus
modern observing facilities.
Shulyak D., Paladini C., Li Causi G., Perraut K., Kochukhov O.
<Mon. Not. R. Astron. Soc., 443, 1629-1642 (2014)>
=2014MNRAS.443.1629S 2014MNRAS.443.1629S
ADC_Keywords: Stars, peculiar ; Interferometry
Keywords: techniques: interferometric - stars: atmospheres -
stars: chemically peculiar - stars: individual: eps UMa
Abstract:
By means of numerical experiments we explore the application of
interferometry to the detection and characterization of abundance
spots in chemically peculiar (CP) stars using the brightest star
ε UMa as a case study. We find that the best spectral regions
to search for spots and stellar rotation signatures are in the visual
domain. The spots can clearly be detected already at a first
visibility lobe and their signatures can be uniquely disentangled from
that of rotation. The spots and rotation signatures can also be
detected in near-infrared at low spectral resolution but baselines
longer than 180m are needed for all potential CP candidates.
According to our simulations, an instrument like VEGA (or its
successor e.g. Fibered and spectrally Resolved Interferometric
Equipment New Design) should be able to detect, in the visual, the
effect of spots and spots+rotation, provided that the instrument is
able to measure V2∼10-3, and/or closure phase. In infrared, an
instrument like AMBER but with longer baselines than the ones
available so far would be able to measure rotation and spots. Our
study provides necessary details about strategies of spot detections
and the requirements for modern and planned interferometric facilities
essential for CP star research.
Description:
In Table 2, we summarize the application of modern and planned
interferometric facilities to a sample of CP stars. Majority of stars
in this table are magnetic CP stars listed in Kochukhov & Bagnulo
(2006A&A...450..763K 2006A&A...450..763K, Cat. J/A+A/450/763) with four additional stars
HD 37776, HD 72106, HD 103498, and HD 177410, and five presumably
non-magnetic HgMn stars (shown at the end of the table).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 68 204 Observability of CP stars with modern and
future interferometers
--------------------------------------------------------------------------------
See also:
J/A+A/450/763 : Evolutionary state of magnetic CP stars (Kochukhov+, 2006)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Pec [MH] M for magnetic CP or H for HgMn star
3- 8 I6 --- HD HD number
10- 13 F4.2 mag Vmag [1.7/9.4] V magnitude
15- 18 F4.2 mag Jmag ?=- J magnitude
20- 23 F4.2 mag Hmag ?=- H magnitude
25- 28 F4.2 mag Kmag ?=- K magnitude
30- 34 F5.1 pc Dist [16/493]?=- Distance
36- 39 F4.2 Rsun Rad [0.6/9.6] Star radius
41- 44 F4.2 mag Diam ?=- Angular diameter
46- 49 I4 m Bmax1 [0/2560] Value of maximum baseline length
needed to fully resolve the star at 0.55um
51- 54 I4 m Bmax2 [0/5818] Value of maximum baseline length
needed to fully resolve the star at 1.25um
56- 59 I4 m Bmax3 [0/7680] Value of maximum baseline length
needed to fully resolve the star at 1.65um
61- 65 I5 m Bmax4 [0/10007] Value of maximum baseline length
needed to fully resolve the star at 2.15um
67- 68 I2 --- Ref [1/10] Reference (1)
--------------------------------------------------------------------------------
Note (1): References as follows:
1 = Kochukhov & Bagnulo, 2006A&A...450..763K 2006A&A...450..763K, Cat. J/A+A/450/763
2 = Khokhlova et al., 2000AstL...26..177K 2000AstL...26..177K
3 = Folsom et al., 2008CoSka..38..245F 2008CoSka..38..245F
4 = Pandey et al., 2011MNRAS.417..444P 2011MNRAS.417..444P
5 = Pandey et al., 2011MNRAS.417..444P 2011MNRAS.417..444P
6 = Adelman et al., 2002ApJ...575..449A 2002ApJ...575..449A
7 = Makaganiuk et al., 2012A&A...539A.142M 2012A&A...539A.142M
8 = Makaganiuk et al., 2011A&A...529A.160M 2011A&A...529A.160M
9 = Kochukhov et al., 2011A&A...534L..13K 2011A&A...534L..13K
10 = Folsom et al. , 2010MNRAS.407.2383F 2010MNRAS.407.2383F
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Apr-2015