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PlanetFU Ori b

Detailed information about planet FU Ori b and its parameters.

Planet parameters Publications Observability Predictor

Planet

Name
FU Ori b
Planet Status
Candidate
    Discovered in
    2023
      Publication
      Status
      Published in a refereed paper
        Update
        2024-06-19
          Mass
          Mass*sin(i)
            Semi-Major Axis
            Orbital Period
            10.6 day
              Eccentricity
                Angular distance
                  ω
                    Tperi
                      Radius
                      Inclination
                        Detection Method
                        Kinematic, Other
                          Mass Meas. Method
                            Radius Meas. Method
                              Primary transit
                                Secondary transit
                                  λ
                                    Impact Parameter b
                                      Time Vr=0
                                        Velocity Semiamplitude K
                                          Calculated temperature
                                            Measured temperature
                                              Hottest point longitude
                                                Geometric albedo
                                                  Surface gravity log(g/gH)
                                                    Alternate Names
                                                      Data SourceTypeResult ValueResult FigureNotesReference
                                                      MoleculeData SourceTypeResult ValueResult FigureNotesReference

                                                      No remarks

                                                      No link

                                                      Star

                                                      Name
                                                      FU Ori
                                                      Distance
                                                      Spectral type
                                                      K0
                                                        Apparent magnitude V
                                                        9.6
                                                          Apparent magnitude I
                                                            Apparent magnitude J
                                                              Apparent magnitude H
                                                                Apparent magnitude K
                                                                  Mass
                                                                  0.6 MSun
                                                                    Age
                                                                      Effective temperature
                                                                      Radius
                                                                      Metallicity [Fe/H]
                                                                      Detected Disc
                                                                        Magnetic Field
                                                                          RA2000
                                                                          05:45:22.4
                                                                            Dec2000
                                                                            +09:04:12.3
                                                                              Alternate Names
                                                                              NOVA Ori 1939, BD+09 5427, HBC 186

                                                                                No remarks

                                                                                No link


                                                                                Related publications

                                                                                • Thermal Evolution and Mass Loss on Short-Period, Low-Mass Planets During FU Orionis Outbursts

                                                                                  BECKER J. & BATYGIN K.
                                                                                  PASP , 137 , 054403
                                                                                  paper  arxiv

                                                                                • On the origin of accretion bursts in FU Ori

                                                                                  NAYAKSHIN, S., ELBAKYAN, V.
                                                                                  MNRAS , 528 , 2182-2198
                                                                                  paper  arxiv  

                                                                                • Extreme evaporation of planets in hot thermally unstable protoplanetary discs: the case of FU Ori

                                                                                  NAYAKSHIN S., OWEN J. & ELBAKYAN V.
                                                                                  MNRAS , 523 , 385
                                                                                  paper  arxiv  

                                                                                • The Revised TESS Input Catalog and Candidate Target List

                                                                                  STASSUN K., OELKERS R., PAEGERT M., TORRES G., PEPPER J. et al.
                                                                                  Astron. J. , 158 , 138
                                                                                  paper  arxiv  

                                                                                • FU Orionis resolved by infrared long baseline interferometry at a 2-AU scale

                                                                                  MALBET F., BERGER J-P., COLAVITA M., KORESKO C., BEICHMAN C., et al.
                                                                                  ApJ. Letters , 507 , 149
                                                                                  paper


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