Ap stars with resolved magnetically split lines: Magnetic field determinations from Stokes I and V spectra

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Table 19

Ap stars with published reliable orbital and rotation periods, not known to show magnetically resolved lines.


HD/HDE	Other id.	Sp. type	P_rot	Ref.	P_orb	e	f(M)	Ref.
			(d)		(d)		(M_⊙)


5550	HR 273	A0p Sr	6.84	1	6.82054	0.006	^a	1 2
8441	BD + 42 293	A2p Sr	69.2	3	106.357	0.122	0.209	4
15089	ι Cas	A4p Sr	1.74050	5	17200	0.626	^b	6
25267	τ⁹ Eri	A0p Si	5.954	7	5.9538	0.13	0.00414	8
25823	HR 1268	B9p SrSi	7.227	9	7.227424	0.18	0.0033	10
98088	HR 4369	A8p SrCrEu	5.9051	11	5.9051	0.1840	^c	11
123335	HR 5292	Bp He wk SrTi	55.215	12	35.44733	^d	^d	12
125248	CS Vir	A1p EuCr	9.295	13	1607	0.21	0.065	14
184471	BD + 32 3471	A9p SrCrEu	50.8	15	429.17	0.2017	0.86	2
191654	BD + 15 4071	A2p SrCr	1.857	16	2121	0.48	0.00140	2
216533	BD + 58 2497	A1p SrCrSi	17.2	17	1413.1	0.437	0.0137	2
219749	HR 8861	B9p Si	1.61887	18	48.304	0.50	0.0554	19

Notes.

^(a)

SB2: M₁ sin³i = 0.1081 M_⊙, M₂ sin³i = 0.0692 M_⊙.

^(b)

Visual binary: M₁ = 1.99 M_⊙, M₂ = 0.69 M_⊙ (based on Hipparcos parallax).

^(c)

SB2: M₁ sin³i = 1.772 M_⊙, M₂ sin³i = 1.290 M_⊙.

^(d)

Eclipsing binary.

Reference. (1) Alecian et al. (2016); (2) Carrier et al. (2002); (3) Aurière et al. (2007); (4) North et al. (1998); (5) Musielok et al. (1980); (6) Drummond et al. (2003); (7) Borra & Landstreet (1980); (8) Leone & Catanzaro (1999); (9) Wolff (1973); (10) Abt & Snowden (1973); (11) Folsom et al. (2013a); (12) Hensberge et al. (2007); (13) Mathys (1991); (14) Hockey (1969); (15) Kudryavtsev & Romanyuk (2012); (16) Vetö et al. (1980); (17) Floquet (1977); (18) Adelman (2000b); (19) Ouhrabka & Grygar (1979).

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