Table 2
Adopted and estimated parameters of the observed bow shock around the runaway stars.
| Runaway | 1 | b | Vw | ![Mathematical equation: $\[\dot{M}\]$](/articles/aa/full_html/2026/05/aa59021-26/aa59021-26-eq14.png) |
![Mathematical equation: $\[\mathrm{n}_{\text {ISM}}^{\mathrm{BS}}\]$](/articles/aa/full_html/2026/05/aa59021-26/aa59021-26-eq15.png) |
![Mathematical equation: $\[\mathrm{n}_{\text {ISM}}^{\mathrm{St}}\]$](/articles/aa/full_html/2026/05/aa59021-26/aa59021-26-eq16.png) |
RSt | R |
|---|---|---|---|---|---|---|---|---|
| − | (deg) | (deg) | (km s−1) | (M⊙ yr−1) | (cm−3) | (cm−3) | (°) | (arcsec) |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
| CD-41 4637 | 263.02 | 2.30 | 2250(e) | 6.9 × 10−6(e) | 30 | 28 | 0.26 | 90 |
| HD 77581/Vela X-1 | 263.06 | 3.93 | 700(a) | 6.3 × 10−7(a) | 1.0 | 3.7 | 0.27 | 53 |
| HD 75860 | 264.14 | 0.27 | (700–800)(d) | (1.6 × 10−7–7.6 × 10−6)(d) | (0.6–34) | 4.3 | 0.08 | 59 |
| HD 76031 | 264.50 | 0.30 | (300–1200)(f) | (10−9–10−8)(f) | (0.7–26) | 17 | 0.05 | 11 |
| CD-444967 | 266.01 | 0.00 | − | − | − | − | 0.18 | 29 |
| CD-47 4564 | 268.46 | −1.65 | (900–1100)(d) | 6.4 × 10−8(d) | (31–38) | 13 | 0.07 | 8** |
| HD 77207 | 268.96 | −1.90 | 500(b) | 1.5 × 10−7(b) | 35 | − | 0.10 | 32 |
| CPD-47 3051 | 269.21 | −0.91 | 1200(b) | 7.7 × 10−9(b) | 13.5 | 14 | 0.10 | 28 |
| HD 298310 | 272.58 | −1.72 | 1200(b) | 3.4 × 10−7(b) | 4.0 | 8.2 | 0.16 | 21 |
| CD-42 4694 | 263.61 | 0.55 | (1140–1300)(e) | (10−7–10−9)(e) | (0.3–25) | 70 | 0.05 | 18 |
| CD-45 4447 | 265.18 | −2.26 | (1745–2390)(c) | (3.6 × 10−8–1.1 × 10−7)(d) | (130–560) | 91 | 0.02 | 22** |
| GSC 08152-02059 | 265.88 | −0.39 | − | − | − | − | 0.06 | 15** |
| HD 78958 | 266.47 | 2.73 | (500–2000)(c) | 3.0 × 10−6(e) | (809–3236)? | 14 | 0.10 | 40** |
| DR3 N72 | 269.01 | −0.76 | − | − | − | − | 0.13 | 34** |
| DR3 N60 | 270.91 | −0.73 | − | − | − | − | 0.10 | 19** |
| HD 298353 | 273.12 | −1.96 | 2500(b) | 6.0 × 10−8(b) | 25 | 41 | 0.10 | 32 |
Notes. (1) name of star, (2), (3) Galactic coordinates of star, (4) adopted terminal wind velocity, (5) adopted mass-loss rate, (6) ambient interstellar number density determined by the balance between the ram pressures of the wind and the ambient medium (Baranov et al. 1971) computed in this work, (7) ambient interstellar number density determined by the relationship of Lequeux (2005) computed in this work, (8) the putative Strömgren radius obtained from WISE 22 μm image of the region, (9) standoff distance from Kobulnicky et al. (2016). The parameters are taken from Giménez-García et al. (2016) (a); Kobulnicky et al. (2019) (b); Prinja et al. (1990) (c); the parameters are based on the spectral type Kobulnicky et al. (2019) (d); Mokiem et al. (2007) (e); typical value for early-B subgiants Krtička (2014) (f); (**) we measured the standoff distance in the WISE 22 μm images. Two objects are indicated as DR3 N72 and N60 based on their last numbers of source_id from Gaia DR3. Suspicious results are in italic. Candidate runaway systems are listed in the bottom part of the table.
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