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Table A.2

Data for the calculation of the KNN FIP bias.

Star Corona Photosphere FIP bias Corona
[C/Fe] [N/Fe] [O/Fe] [Ne/Fe] [C/Fe] [N/Fe] [O/Fe] [Ne/Fe] source
AD Leo 1.45 0.96 1.64 1.18 0.58 0.33 0.87 0.48 0.74 ± 0.10 (1)
CN Leo 1.25 0.64 1.33 0.76 0.53 0.32 0.84 0.80 0.46 ± 0.32 (2) Table 2 DEM1
EQ Peg A – 0.80 1.68 1.17 – 0.32 0.84 0.80 0.65 ± 0.25 (3) Table 7 Q
EQ Peg B – 0.82 1.61 1.13 – 0.32 0.84 0.80 0.61 ± 0.22 (3) Table 7 Q
Prox Cen – 1.13 1.54 1.04 – 0.32 0.84 0.80 0.67 ± 0.31 (3) Table 10 Q
EV Lac – 0.93 1.69 1.10 – 0.32 0.91 0.80 0.65 ± 0.24 (3)Table 10 Q
YY Gem – 1.12 1.75 1.26 – 0.32 0.86 0.80 0.80 ± 0.23 (3) Table 10 Q
AU Mic 1.63 1.19 1.77 1.39 0.57 0.32 0.88 0.49 0.93 ± 0.08 (1)
AT Mic 1.42 0.82 1.55 1.16 0.52 0.32 0.84 0.80 0.70 ± 0.24 (4) Table 4 3T model
AB Dor 1.50 1.06 1.75 1.35 0.89 0.36 1.43 1.04 0.49 ± 0.20 (1)
LO Peg 1.50 0.84 1.61 1.35 1.07 0.23 1.69 0.80 0.46 ± 0.31 (5) Table 1 Q
V471 Tau – – 1.57 1.43 – – 1.25 0.86 0.53 ± 0.17 (6) Table 4
36 Oph A 0.57 0.44 1.19 0.88 0.90 0.37 1.47 1.08 − 0.18 ± 0.18 (1)
36 Oph B 0.44 0.33 1.10 0.67 0.87 0.37 1.41 1.02 − 0.28 ± 0.17 (1)
ξ Boo B 0.78 – 1.19 0.97 0.68 0.31 1.08 0.70 0.16 ± 0.10 (1)
61 Cyg A 0.95 0.34 1.12 0.79 0.70 0.29 1.14 0.76 0.08 ± 0.12 (1)
61 Cyg B 1.26 – 1.60 1.06 0.61 0.33 1.04 0.66 0.54 ± 0.12 (1)
70 Oph A 0.64 0.18 0.92 0.56 0.80 0.41 1.30 0.92 − 0.28 ± 0.11 (1)
70 Oph B 0.98 0.70 1.35 1.01 0.69 0.35 1.08 0.70 0.31 ± 0.04 (1)
ϵ Eri 0.90 0.42 1.20 0.84 0.83 0.39 1.34 0.96 − 0.04 ± 0.11 (1)
α Cen A 0.72 0.06 0.35 0.41 0.83 0.52 1.22 0.84 − 0.47 ± 0.31 (1) low activity
α Cen B 0.70 0.14 0.87 0.33 0.79 0.54 1.21 0.83 − 0.33 ± 0.17 (1) low activity
π1 UMa 0.54 0.36 0.84 0.48 0.91 0.37 1.30 0.91 − 0.32 ± 0.21 (1)
EK Dra 0.98 0.19 1.12 0.96 0.84 0.39 1.29 0.90 − 0.04 ± 0.17 (1)
ξ Boo A 0.75 0.20 1.11 0.69 0.85 0.38 1.34 0.95 − 0.19 ± 0.07 (1)
χ1 Ori 0.35 − 0.33 0.64 0.88 0.91 0.36 1.28 0.89 − 0.39 ± 0.31 (7)
κ Cet 0.42 − 0.12 0.67 1.00 0.84 0.39 1.29 0.91 − 0.28 ± 0.32 (7)
β Com 0.49 − 0.53 0.59 0.46 0.92 0.36 1.27 0.88 − 0.52 ± 0.23 (7)
47 Cas B 0.83 0.39 1.03 1.42 0.86 0.39 1.29 0.90 0.14 ± 0.33 (7)
ι Hor 0.75 0.43 1.31 1.18 0.88 0.44 1.25 0.86 0.15 ± 0.19 (8)
11 LMi 0.97 0.11 1.09 0.33 0.78 0.58 1.18 0.80 − 0.12 ± 0.32 (9) Table 3
HR 7291 – – 0.68 0.13 – – 1.25 0.80 − 0.53 ± 0.08 (9) Table 4
σ2 CrB – 0.35 1.17 0.74 – 0.40 1.28 0.80 0.01 ± 0.03 (10) Table 5 Q
ξ UMa – – 1.42 1.50 0.94 0.34 1.34 0.96 0.39 ± 0.33 (11) Table 3
HR 1099 1.50 1.16 1.87 1.41 0.78 0.45 1.19 0.80 0.76 ± 0.05 (12) Table 4 APEC
UX Ari 1.95 1.72 2.03 1.72 0.80 0.45 1.21 0.80 1.12 ± 0.21 (12) Table 4 APEC
λ And 1.28 0.74 1.67 1.31 0.87 0.37 1.38 0.80 0.48 ± 0.09 (12) Table 4 APEC
VY Ari 1.57 1.11 1.78 1.44 0.80 0.43 1.22 0.80 0.75 ± 0.09 (12) Table 4 APEC
Capella 0.66 0.40 0.93 0.40 0.62 0.64 1.09 0.80 − 0.11 ± 0.19 (12) Table 4 APEC
σ Gem – 1.21 1.61 1.24 – 0.48 1.22 0.80 0.60 ± 0.19 (13) Table 4
31 Com – – 1.31 0.66 – – 1.24 0.80 0.05 ± 0.15 (14) Table 5
μ Vel – – 1.06 0.44 – – 1.16 0.80 − 0.15 ± 0.18 (14) Table 5, ObsID 3410
β Cet – – 1.13 0.54 – – 1.10 0.80 − 0.03 ± 0.21 (14) Table 5
FK Com – – 1.35 1.06 – – 1.17 0.80 0.30 ± 0.06 (15) Table 7
YY Men 1.14 1.19 1.41 1.13 0.81 0.45 1.26 0.80 0.47 ± 0.25 (16) Table 2 XMM Method 1
EI Eri 1.03 0.58 1.34 1.27 0.77 0.46 1.21 0.82 0.32 ± 0.15 (17) Figure 5
V851 Cen 1.19 1.05 1.84 1.89 0.80 0.44 1.24 0.85 0.74 ± 0.27 (18) Table 2
AR Psc 1.74 1.00 1.70 1.57 0.67 0.54 1.09 0.70 0.83 ± 0.27 (19) Table 5
AY Cet 1.70 1.01 1.37 1.35 0.76 0.51 1.27 0.88 0.59 ± 0.34 (19) Table 5
II Peg – 1.33 2.47 2.32 0.88 0.34 1.38 0.99 1.22 ± 0.17 (20) Table 4 Q
AR Lac – 0.93 1.51 1.48 0.94 0.34 1.38 1.00 0.49 ± 0.25 (21) Table 3
η Lep 0.78 – 1.09 0.55 1.03 0.33 1.35 0.96 − 0.30 ± 0.09 (1)
π3 Ori 0.79 0.11 0.92 0.46 0.99 0.33 1.30 0.91 − 0.31 ± 0.12 (1)
τ Boo A 0.83 – 0.91 0.50 0.95 0.41 1.24 0.85 − 0.27 ± 0.13 (1)
Procyon 1.20 0.68 1.43 0.77 0.98 0.35 1.29 0.80 0.25 ± 0.15 (22) Table 4
Altair 0.95 0.32 0.96 0.64 1.07 0.30 1.42 1.42 − 0.25 ± 0.36 (23) Table 2 MOS/RGS

Notes. Coronal abundances are taken in quiescent (Q) or low-activity state, where available. The photospheric abundances are predicted with the KNN method using data from Wang et al. (2020), and are relative to Asplund et al. (2009) solar composition and Ne from Drake & Testa (2005). As there were no Ne abundances in the LAMOST dataset, the photospheric [Ne/Fe] column was calculated as [Ne/Fe]phot =[O/Fe]phot + log100.41. The FIP bias and its uncertainty are calculated as the mean and standard deviation of [X/Fe]cor−[X/Fe]phot, where X can be C, N, O, and Ne. The FIP bias column is corrected by +0.084 according to Wood et al. (2018), except for the stars listing (1) as the source. As discussed in Sect. 2, GJ 338 AB is omitted.

References. (1) Wood et al. (2018), (2) Fuhrmeister et al. (2007), (3) Liefke et al. (2008), (4) Robrade & Schmitt (2005), (5) Lalitha et al. (2017), (6) García-Alvarez et al. (2005), (7) Telleschi et al. (2005), (8) Sanz-Forcada et al. (2019), (9) Peretz et al. (2015), (10) Osten et al. (2003), (11) Ball et al. (2005), (12) Audard et al. (2003), (13) Huenemoerder et al. (2013), (14) García-Alvarez et al. (2006), (15) Gondoin et al. (2002), (16) Audard et al. (2004), (17) Nordon et al. (2013), (18) Sanz-Forcada et al. (2004), (19) Sanz-Forcada et al. (2009), (20) Huenemoerder et al. (2001), (21) Huenemoerder et al. (2003), (22) Raassen et al. (2002), (23) Robrade & Schmitt (2009)

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