2018A&A...616A..77B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST17:22:30

2018A&A...616A..77B - Astronomy and Astrophysics, volume 616A, 77-77 (2018/8-1)

K2 space photometry reveals rotational modulation and stellar pulsations in chemically peculiar A and B stars.

BOWMAN D.M., BUYSSCHAERT B., NEINER C., PAPICS P.I., OKSALA M.E. and AERTS C.

Abstract (from CDS):


Context. The physics of magnetic hot stars and how a large-scale magnetic field affects their interior properties is largely unknown. Few studies have combined high-quality observations and modelling of magnetic pulsating stars, known as magneto-asteroseismology, primarily because of the dearth of detected pulsations in stars with a confirmed and well-characterised large-scale magnetic field.
Aims. We aim to characterise observational signatures of rotation and pulsation in chemically peculiar candidate magnetic stars using photometry from the K2 space mission. Thus, we identify the best candidate targets for ground-based, optical spectropolarimetric follow-up observations to confirm the presence of a large-scale magnetic field.
Methods. We employed customised reduction and detrending tools to process the K2 photometry into optimised light curves for a variability analysis. We searched for the periodic photometric signatures of rotational modulation caused by surface abundance inhomogeneities in 56 chemically peculiar A and B stars. Furthermore, we searched for intrinsic variability caused by pulsations (coherent or otherwise) in the amplitude spectra of these stars.
Results. The rotation periods of 38 chemically peculiar stars are determined, 16 of which are the first determination of the rotation period in the literature. We confirm the discovery of high-overtone roAp pulsation modes in HD 177765 and find an additional 3 Ap and Bp stars that show evidence of high-overtone pressure modes found in roAp stars in the form of possible Nyquist alias frequencies in their amplitude spectra. Furthermore, we find 6 chemically peculiar stars that show evidence of intrinsic variability caused by gravity or pressure pulsation modes.
Conclusions. The discovery of pulsations in a non-negligible fraction of chemically peculiar stars make these stars high-priority targets for spectropolarimetric campaigns to confirm the presence of their expected large-scale magnetic field. The ultimate goal is to perform magneto-asteroseismology and probe the interior physics of magnetic pulsating stars.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: chemically peculiar - stars: magnetic field - stars: rotation - stars: oscillations - stars: early-type

Status at CDS:   Objects in title, abstract, text, figures, and all or part of small table(s) being processed in SIMBAD.

Simbad objects: 70

goto Full paper

goto View the reference in ADS

Number of rows : 70

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* V1137 Tau a2* 04 12 51.2453721747 +22 24 48.462108078 6.04 6.31 6.12     B8III 98 0
2 HD 284639 * 04 45 59.1994877195 +23 55 00.584436702   10.13 9.68     A0 8 0
3 V* V901 Ori Ro* 05 40 56.3704270929 -01 30 25.856714776 5.96 6.82 6.96     B2V 294 2
4 EPIC 202061263 * 06 03 08.820 +23 47 23.71           ~ 1 0
5 HD 41641 dS* 06 06 40.5781479152 +06 43 49.891916932   8.14 7.86     A5III 18 0
6 [M67b] +22 562 ** 06 07 54.59 +22 13 57.2     11.3     B9p 7 0
7 HD 43317 Pu* 06 15 47.0136233779 +04 17 01.097508973 5.82 6.456 6.614     B3IV 90 0
8 HD 255134 * 06 19 53.7083627500 +23 15 54.426696450 9.01 9.46 9.18     B1IVp 13 0
9 HD 51452 Be* 06 57 20.6218635204 -04 11 37.421822446 7.51 8.21 8.08     B7Ib/II 40 0
10 NGC 2682 OpC 08 51 18 +11 48.0           ~ 2032 0
11 HD 97859 * 11 15 30.8973562469 +04 57 23.500125864 8.695 9.238 9.352 9.387 9.441 ~ 42 0
12 HD 107000 * 12 18 19.1137192344 +03 06 04.069049711   8.21 8.02     A3IV 20 0
13 V* CU Vir a2* 14 12 15.8054758 +02 24 33.953395 4.46 4.90 5.02 5.10 5.23 ApSi 347 0
14 V* V913 Sco Ro* 15 58 34.8664705139 -24 49 53.358222372 4.70 5.34 5.43     B5V 177 0
15 HD 145792 a2* 16 13 45.49839 -24 25 19.5421         6.14 B6IV 113 0
16 V* V933 Sco a2* 16 20 05.4924613867 -20 03 23.032932987   7.56 7.40     B9II/III 173 0
17 V* V955 Sco a2* 16 39 31.5585248587 -27 17 08.165524396   8.92 8.71     ApCrEuSr 46 0
18 HD 152366 * 16 53 57.7036221447 -25 04 09.283440703   8.11 8.08     ApSi 22 0
19 HD 152834 a2* 16 56 58.0232819602 -26 57 05.598985401   8.85 8.83     ApSi 13 0
20 HD 153192 a2* 16 59 05.5224026128 -27 04 55.154034810   10.12 10.08     ApEuCr(Sr) 8 0
21 HD 153997 a2* 17 03 36.2614069999 -19 27 43.800997885   9.56 9.50     ApSi 10 1
22 HD 155127 a2* 17 10 52.1368040965 -26 27 06.081207358   8.59 8.38     ApEuCr 19 0
23 HD 158336 a2* 17 29 26.7030403978 -18 39 51.201251574   9.49 9.36     ApSi 13 0
24 HD 158596 a2* 17 31 03.4621524 -21 29 07.037487   9.45 9.53 9.67   ApSi 21 0
25 HD 161342 * 17 46 01.0009840898 -22 37 30.581802608   8.95 8.66     B8III(pSi) 5 0
26 HD 161851 * 17 49 00.4165753960 -25 44 58.350722330   8.72 8.61     ApSi 9 0
27 HD 162759 * 17 53 36.1172640330 -24 26 06.663376379   10.41 10.10     ApSi 6 0
28 HD 162814 * 17 53 53.8141587805 -23 22 30.436652276   10.86 10.24     ApSi 7 0
29 V* V2052 Oph bC* 17 56 18.3998830562 +00 40 13.276647618 5.28 5.874 5.820     B3III 197 0
30 HD 164085 a2* 18 00 12.0155037302 -17 05 20.522080509   10.42 10.19     ApSi 7 0
31 CCDM J18004-2258B * 18 00 23.3863991823 -22 58 03.232695921     12.4     ~ 1 0
32 HD 164068 * 18 00 24.1458248984 -22 57 52.095733859   10.04 9.90     ApSi 7 0
33 HD 164190 * 18 00 51.5247373976 -18 58 04.120010128   9.37 9.13     ApSi 6 0
34 HD 164224 * 18 00 57.6151170527 -20 59 17.211385460   8.67 8.49     ApSiCr 18 0
35 HD 165321 * 18 06 29.7734175876 -24 09 32.987135947   9.13 8.97     A0V(pSi) 11 0
36 HD 165945 * 18 09 02.1211555456 -15 31 42.158545059   9.67 9.41     ApSrEuCr 10 0
37 HD 165972 a2* 18 09 32.5985504227 -24 39 49.930679675   9.02 8.96     B9II(pSi) 11 0
38 HD 166190 * 18 10 21.9355640247 -21 16 35.156141565   10.01 9.81     A(pSi) 5 0
39 HD 166542 * 18 11 51.9585097447 -18 28 52.133266377   9.92 9.94     ApSi 6 0
40 HD 166804 a2* 18 13 03.3926237034 -18 18 44.209185247   8.84 8.90     ApSi 8 0
41 HD 167700 * 18 17 24.8532956564 -24 24 04.423920544   9.87 9.54     ApSrEu(Cr) 5 0
42 HD 168187 * 18 19 17.7491023062 -18 19 55.162216925   10.06 10.02     B8/9Ib/II(pSi) 5 0
43 HD 172480 a2* 18 41 24.6860866814 -23 55 20.891367131   10.22 10.09     ApSi 11 0
44 V* V4404 Sgr a2* 18 45 53.2296563172 -18 21 50.634192457   7.51 7.43     ApSi 20 0
45 HD 173657 a2* 18 47 37.1494519578 -28 16 46.965444312   7.48 7.41     ApSiCr 18 0
46 HD 173857 * 18 48 34.7568404285 -27 06 56.942490581   10.44 10.40     ApSiCr(Sr) 6 0
47 HD 174146 a2* 18 50 05.2795717556 -24 14 02.392727599   10.56 10.03     ApSi(Cr) 8 0
48 HD 174356 a2* 18 51 08.6097629190 -24 23 14.531127339   9.37 9.18     ApSi 9 0
49 HD 174648 * 18 51 41.0001981972 -01 45 35.240841550   8.90 8.81     B9.5V 13 0
50 HD 176330 * 19 00 26.9044935873 -18 05 44.148653683   10.54 10.39     ApSi 7 0
51 HD 177013 * 19 03 27.0017635858 -17 18 36.037737298   9.34 9.04     ApEu 9 0
52 HD 177016 * 19 03 40.5685685580 -20 34 36.920314990   9.67 9.34     ApEuSrCr 12 0
53 HD 177562 * 19 06 19.2447333653 -27 17 13.508058929   7.39 7.38     ApSi 12 0
54 HD 177765 * 19 07 09.7792915616 -26 19 54.507708452   9.60 9.15     ApSrEuCr 28 0
55 HD 178786 * 19 10 58.8363901208 -25 40 19.720588039   10.20 10.24     ApSi(Cr) 9 0
56 HD 180303 ** 19 16 46.8136183737 -20 46 35.155123985   9.50 9.48     ApSi 11 0
57 HD 181004 * 19 19 23.4138372695 -16 57 16.389660676   9.54 9.64     B8III(pSi) 8 0
58 V* V694 Lyr * 19 20 30.7975651366 +37 50 55.028480290     14.210   13.830 ~ 3 0
59 HD 181810 * 19 22 43.5663967072 -21 25 27.519090070   10.65 10.66     ApEuCrSr 7 0
60 HD 182459 * 19 25 40.1553236794 -23 08 12.172147751   9.52 9.59     ApSi 8 0
61 HD 184343 * 19 34 51.5497719180 -23 22 29.425876954   10.10 9.74     FpSrCrEu 6 0
62 HD 188774 dS* 19 55 10.0376514155 +41 17 10.270913232   9.05 8.81     A7.5IV-III4A8IIIs 27 0
63 HD 200405 SB* 21 01 38.2996945581 +47 54 47.267062295   8.98 8.90     A0pSrCr 35 0
64 * bet Cep bC* 21 28 39.5968513 +70 33 38.574681 2.05 3.01 3.23 3.33 3.55 B0.5IIIs 683 0
65 * e Aqr * 22 10 37.4820650 -11 33 53.775377   5.299 5.422     B5III 84 0
66 * rho Aqr SB* 22 20 11.9183032023 -07 49 15.974185849 4.94 5.286 5.339     B8III 76 0
67 V* GL Lac a2* 22 44 07.5047921489 +55 35 21.208257555   8.85 8.81     A0p 261 0
68 * tau01 Aqr * 22 47 42.7699558802 -14 03 23.141882884   5.650 5.681   5.67 B9V 52 0
69 HD 219831 * 23 19 01.4363329461 -09 03 35.044779480   10.20 9.99     ApSr(Cr) 8 0
70 HD 220556 * 23 24 44.2649795755 -06 00 43.034855356   10.198 9.850     ApSrEuCr 5 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2018A&A...616A..77B and select 'bookmark this link' or equivalent in the popup menu


2020.07.14-17:22:30

© Université de Strasbourg/CNRS

    • Contact