Table 1.
Known ssrAp stars.
| HD/HDE | Other ID | Spectral type | Prot (d) | Reference | B0 (kG) | roAp |
|---|---|---|---|---|---|---|
| Stars with accurately determined periods | ||||||
| 50169 | BD−1 1414 | A3p SrCrEu | 10600 | Mathys et al. (2019a) | 5.1 | |
| 9996 | HR 465 | B9p CrEuSi | 7937 | Metlova et al. (2014) | 4.7 | |
| 965 | BD−0 21 | A8p SrEuCr | 6030 | Mathys et al. (2019b) | 4.3 | |
| 166473 | CoD−37 12303 | A5p SrEuCr | 3836 | Mathys et al. (2020a) | 7.1 | roAp |
| 94660 | HR 4263 | A0p EuCrSi | 2800 | Mathys (2017) | 6.2 | |
| 187474 | HR 7552 | A0p EuCrSi | 2345 | Mathys (1991) | 5.4 | |
| (a) | CPD−62 2717 | B8 (b) | 1765 | Chojnowski et al. (2023) | 9.9 | |
| 59435 | BD−8 1937 | A4p SrCrEu | 1360 | Wade et al. (1999) | 3.0 | |
| 18078 | BD+55 726 | A0p SrCr | 1358 | Mathys et al. (2016) | 3.4 | |
| 93507 | CPD−67 1494 | A0p SiCr | 556 | Mathys et al. (1997) | 7.2 | |
| 2453 | BD+31 59 | A1p SrEuCr | 518.2 | Pyper & Adelman (2017) | 3.7 | |
| 51684 | CoD−40 2796 | F0p SrEuCr | 371 | Mathys (2017) | 6.0 | |
| 61468 | CoD−27 4341 | A3p EuCr | 322 | Mathys (2017) | 6.8 | |
| 110274 | CoD−58 4688 | A0p EuCr | 265.3 | Freyhammer et al. (2008) | 4.0 | |
| 69544 | CD −50 3225 | B8p Si | 236.5 | Bernhard et al. (2015a) | ||
| 188041 | HR 7575 | A6p SrCrEu | 223.78 | Mathys (2017) | 3.7 | |
| 221568 | BD+57 2758 | A1p SrCrEu | 159.10 | Pyper & Adelman (2017) | ||
| 66821 | CPD−54 1483 | A0p Si | 154.9 | Bernhard et al. (2015a) | ||
| 116458 | HR 5049 | A0p EuCr | 148.39 | Mathys (2017) | 4.7 | |
| 126515 | BD+1 2927 | A2p CrSrEu | 129.95 | Mathys et al. (1997) | 12.7 | |
| 340577 | BD+25 4289 | A3p SrCrEu | 116.7 | Hümmerich et al. (2016) | ||
| 263361 | BD+19 1468 | B9p Si | 88.9 | Bernhard et al. (2015a) | ||
| 149766 | CD−51 10384 | B8p Si | 87.3 | Bernhard et al. (2015a) | ||
| (c) | BD−7 1884 | SrCrEu | 75.97 | Hümmerich et al. (2016) | ||
| 158919 | CPD−65 3465 | B9p Si | 75.72 | Bernhard et al. (2015a) | ||
| 102797 | CPD−75 757 | B9p Si | 75.02 | Koen & Eyer (2002) | ||
| 8441 | BD+42 293 | A2p Sr | 69.51 | Pyper & Adelman (2017) | ||
| 5797 | BD+59 163 | A0p CrEuSr | 68.05 | Dukes & Adelman (2018) | ||
| 123335 | HR 5292 | Bp He wk SrTi | 55.215 | Hensberge et al. (2007) | ||
| 103844 | CPD−75 767 | A0p Si | 52.95 | Bernhard et al. (2015a) | ||
| 200311 | BD+43 3786 | B9p SiCrHg | 52.0084 | Wade et al. (1997) | 8.4 | |
| 256476 | TYC 736-1842-1 | A2p Si | 51.23 | Hümmerich et al. (2016) | ||
| 184471 | BD+32 3471 | A9p SrCrEu | 50.8 | Kudryavtsev & Romanyuk (2012) | ||
| 87528 | CPD−62 1415 | B8/9 III (d) | 50.35 | Bernhard et al. (2015a) | ||
| Stars with well-established period lower limits | ||||||
| 201601 | γ Equ | A9p SrEu | ≳35 500 | Bychkov et al. (2016) | 3.9 | roAp |
| 213258 | BD+35 4815 | B9p | ≳18 000 | Mathys et al. (2023) | 3.8 | roAp |
| 116114 | BD−17 3829 | F0p SrCrEu | > 17 700 | Giarrusso et al. (2022) | 6.0 | roAp |
| 101065 | CD−46 7232 | F3p Ho | > 15 700 (e) | Hubrig et al. (2018) | roAp | |
| 55719 | HR 2727 | A3p SrCrEu | > 14 000 | Giarrusso et al. (2022) | 6.3 | |
| 177765 | CD−26 13816 | A5p SrEuCr | > 13 500 | Giarrusso et al. (2022) | 3.4 | roAp |
| 137949 | 33 Lib | F0p SrEuCr | ≫10 000 | Giarrusso et al. (2022) | 4.7 | roAp |
| 165474 | BD+12 3382B | A7p SrCrEu | > 9900 | Giarrusso et al. (2022) | 6.6 | |
| 176232 | 10 Aql | A6p Sr | ≫4400 | Sikora et al. (2019) | roAp | |
| 29578 | CD−54 902 | A4p SrEuCr | ≳4000 (f) | Giarrusso et al. (2022) | 3.1 | |
Notes. Column 1 gives the HD number of the stars (when available) and Col. 2 another identification. The spectral types listed in Col. 3 are from Renson & Manfroid (2009), except when otherwise mentioned in a footnote. Columns 4 and 5 contain the value of the period, when it has been accurately determined, or its lower limit, and the corresponding literature source. For those stars whose spectral lines are resolved into their magnetically split components, the phase-averaged value B0 of the mean magnetic field modulus ⟨B⟩ (the line intensity weighted average over the visible stellar hemishphere of the modulus of the magnetic vector) appears in Col. 6. For stars for which the available ⟨B⟩ measurements sample the full rotation cycle well, B0 is the average of ⟨B⟩ over the rotation period; otherwise, it is an average over the observed phases. Most entries in Col. 6 are from Tables 13 and 14 of Mathys (2017); for a few stars, they are complemented by more recent data from Mathys et al. (2019a,b, 2020a, 2023), Giarrusso et al. (2022), and Chojnowski et al. (2023). Rapidly oscillating Ap (roAp) stars are identified in Col. 7.
Spectral type from Loden et al. (1976).
Spectral type from Houk & Cowley (1975).
We adopted the time base covered by the ⟨Bz⟩ measurements as lower limit, not the heavily extrapolated value of 188 yr proposed by Hubrig et al. (2018).
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