CONFIRMED
MILKY WAY
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| V934 Her | IRAS 17044+2402 | GSC2.4.2 N3F4013953 | AAVSO 000-BCW-066 |
| SIMBAD V* V934 Her | Pan-STARRS 136762566437726815 | SAO 84844 | VSX 15745 |
| GAIA DR3 4571810378118789760 | SkyMapper - | WRAY - | GCVS V0934 Her |
| 2MASS J17063452+2358186 | HIP 83714 | Hen - | BD +24 3121 |
| WISE J170634.51+235818.4 | TYC 2060-757-1 | ESO - | HD 154791 |
| Bidelman (1954) | - | Allen (1984) | - | Belzcyński et al. (2001) | V934 Her (Susp.) |
| Gaposchkin (1957) | - | Kenyon (1986) | - | Akras et al. (2019) | V934 Her (Conf.) |
| Boyarchuk (1969) | - | Vaidis (1988, 1991) | - |
| Right ascension (°) | 256.6438Ref | Parallax (mas) | 1.841±0.051Ref | Reddening E(B-V) (mag) | 0.04±0.0Ref, Note |
| Declination (°) | 23.9718Ref | Distance (kpc) | 0.42±0.04Ref 0.54Ref, Note, 0.53Ref, Note |
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| Galactic longitude (°) | 45.1517Ref | Proper motion in α (mas/yr) | -8.73±0.04Ref | ||
| Galactic latitude (°) | 32.9907Ref | Proper motion in δ (mas/yr) | -5.57±0.05Ref |
| X-Ray | YesRef | IR type | SRef | Radio | NoRef |
| X-Ray type | γRef | J (mag) | 4.17Ref | Flickering | NoRef |
| GALEX FUV (mag) | 18.16Ref | H (mag) | 3.32Ref | Outbursts | - |
| GALEX NUV (mag) | 17.45Ref | K (mag) | 2.99Ref | Outburst type | - |
| IUE | YesRef | WISE W1 (mag) | 2.22Ref | Jets | Yes?Ref |
| FUSE | NoRef | WISE W2 (mag) | 2.85Ref | Resolved nebula | - |
| U (mag) | 11.20Ref | WISE W3 (mag) | 2.96Ref | IPmax (eV) | 77.5 (UV)Ref |
| B (mag) | 9.00Ref | WISE W4 (mag) | 2.84Ref | [O III] lines | NoRef |
| V (mag) | 7.65Ref | IRAS 12μm (Jy) | 2.77Ref | He II lines | NoRef |
| R (mag) | - | IRAS 25μm (Jy) | 0.74Ref | [Fe VII] lines | NoRef |
| I (mag) | - | IRAS 60μm (Jy) | 0.40Ref | O VI lines | NoRef |
| BP (mag) | 7.89Ref | IRAS 100μm (Jy) | 1.00Ref | ||
| G (mag) | 6.75Ref | AKARI S09 (Jy) | 3.59Ref | ||
| RP (mag) | 5.68Ref | AKARI S18 (Jy) | 0.99Ref |
| Orbital period (days) | 4391±33Ref | γ velocity (km/h) | -48.7±0.1Ref, -47.358±0.063Ref, -47.16±0.30Ref |
Size of giant’s orbit (AU) | 0.503Ref |
| Eccentricity | 0.354±0.036Ref | RV of giant (km/h) | 1.915±0.097Ref | Separation (AU) | - |
| Inclination (°) | 11.7±0.4Ref | Inferior conj. of giant (JD) | 2457118 | Mass function | 0.00217Ref |
| Eclipses | - | Mass ratio | 1.19Ref | ||
| Orbital ephemeris | - |
| Spectral type | M3 IIIRef, M2 IIIRef | Mass (M⊙) | 1.6±0.2Ref | Pulsation | YesRef |
| Eff. temperature (K) | 3650±100Ref | Radius (R⊙) | 90±20Ref | Type | SRRef |
| IR type | SRef | Luminosity (L⊙) | 1200±200Ref | Pulsation period (days) | 28.82Ref, 44.08±0.1Ref |
| Metallicity [Fe/H] | -0.6±0.1Ref | Pulsation ephemeris | Max (V) = 2455428.27 + 28.82 x ERef |
| Type/Spectral type | NSRef | Mass (M⊙) | 1.35Ref | Spin period (min) | - |
| Shell-burning/Accreting-only | accreting-onlyRef | Radius (R⊙) | - | Accretion disk | - |
| Eff. temperature (K) | - | Luminosity (L⊙) | - | ||
| Lower limit (K) | - | ||||
| Upper limit (K) | - |
Initially suspected to be a symbiotic star in Garcia et al. (1983), who observed an M-type bright giant with UV emission lines with ionization potential up to 77.5 eV and the absence of optical emission lines. They suggested the model of M II + NS. An X-ray outburst was detected in Tomasella et al. (1997), having no discernible impact on the optical properties. Galloway et al. (2002) revealed a period of 404 days, and Goranskij et al. (2012) suggested that the giant is pulsating. Hinkle et al. (2019) proposed based on infrared observations that the 404-day period is a long secondary period of a pulsating giant. Additionally, the orbital period of the system was determined to be approximately 4391 days using the infrared radial velocities obtained in the same study.