Planet AB And (AB)b

Detailed information about planet AB And (AB)b and its parameters.

Planet parameters Publications Observability Predictor

Planet

Name

AB And (AB)b

Planet Status

Candidate

Discovered in

2025

Publication Status

—

Update

2025-10-27

Mass

—

Mass*sin(i)

8.7

M_J 1 publication

Searching for substellar companion candidates with Gaia: II. A catalog of 9698 planet candidate solar-type hosts

Semi-Major Axis

1.99 AU 1 publication

Searching for substellar companion candidates with Gaia: II. A catalog of 9698 planet candidate solar-type hosts

Orbital Period

—

Eccentricity

—

Angular distance

—

ω

—

T_peri

—

Radius

—

Inclination

—

Detection Method

Astrometry

Mass Meas. Method

—

Radius Meas. Method

—

Primary transit

—

Secondary transit

—

λ

—

Impact Parameter b

—

Time V_r=0

—

Velocity Semiamplitude K

—

Calculated temperature

—

Measured temperature

—

Hottest point longitude

—

Geometric albedo

—

Surface gravity log(g/g_H)

—

Alternate Names

—

Data Source	Type	Result Value	Result Figure	Notes	Reference

Molecule	Data Source	Type	Result Value	Result Figure	Notes	Reference

Given the presence of an unseen, relatively close white dwarf tertiary companion, the circumbinary planet is also a candidate second generation planet.

No link

Star

Name

AB And (AB)

Distance

85.35 pc

Spectral type

G5V+G5V

Apparent magnitude V

9.5

Apparent magnitude I

—

Apparent magnitude J

—

Apparent magnitude H

—

Apparent magnitude K

—

Mass

1.613 (\pm 0.037)

M_Sun 1 publication

Period variation and four color light curves investigation of AB And

Age

—

Effective temperature

5450.0 K 1 publication

Period variation and four color light curves investigation of AB And

Radius

0.822 (\pm 0.023)

R_Sun 1 publication

Period variation and four color light curves investigation of AB And

Metallicity [Fe/H]

—

Detected Disc

—

Magnetic Field

—

RA₂₀₀₀

23:11:32.1

Dec₂₀₀₀

+36:53:35.1

Alternate Names

HIP 114508

Close-in spectroscopic binary (P = 0.3319 d) with an G dwarf secondary (m₁ = 0.579 M_Sol, m₂ = 1.034 M_Sol, r₁ = 0.822 R_Sol, r₂ = 1.15 R_Sol, T₁ = 5450 K, T₂ = 5020 K; Li et al. 2014).
Demircan et al. (1994) suggested that observed period variability may be a result of the orbital motion in a wide triple system and the third body would be a white dwarf (m₃ = 0.4-0.5 M_Sol). Li et al. (2014) confirm the third body hypothesis (P₃ ≈ 106 y, e₃ = 0.41 ± 0.15) whereas Kozyreva et al. (2018) infer the presence of even a fourth body in the system, likely an ultracool M dwarf (m₄ = 0.1 M_Sol, P₄ ≈ 59 y, e₄ = 0.87), although dynamically unstable.