Summary for : (762) Pulcova

DynT.TT.BT T.L B T.DDensity (g/cm^3)Δρ/ρDiameter (km)ΔD/DMass (kg)ΔM/MRefAvg.M
MBAF-C | Cb-1.17 ± 1.78   (E)152 %138.1 ± 7.65.5 %1.62e+18 ± 2.44e+18151 %SEVM
MBAF-C | Cb-1.08 ± 7.89   (E)733 %136.6 ± 5.43.9 %1.44e+18 ± 1.05e+19733 %Sw.avg
MBACb1.00 ± 0.14   (B)14 %138.4 ± 6.04.3 %1.40e+18 ± 1.00e+177 %C?

Average asteroid densities (g/cm^3):
C = 1.3 ± 0.6, B = 2.4 ± 0.5, S = 2.7 ± 0.5, M = 3.5 ± 1.0, P = 2.8 ± 1.6, X = 1.9 ± 0.8, Xc = 4.9 ± 0.9, Xk = 4.2 ± 0.7 (Ref)

Additional resources:
3D Model | JPL New Horizons | Minor Planet Center | Wikipedia (these auto-generated links might not work)

Note: The density estimates have been ranked from (A) to (E), corresponding to the relative error: (B) less than 20%, (C) between 20 and 50%, (D) between 50 and 100%, and (E) more than 100%. (A) stands for (presumably) reliable estimates (accuracy better than 20%), based on more than 5 mass estimates and 5 diameter estimates, or a spacecraft encounter. Apparently unrealistic densities (ρ > 8) are tagged with (X).

EVM: average by using the Expected Value Method (Ref). w.avg: weighted average (with w = 1/err^2).

T.T: Tholen Tax Class. T.B: Bus & Binzel Tax Class. T T.L: S3OS2 Lazarro (Tholen) Tax Class. T.L B: S3OS2 Lazarro (Bus & Binzel) Tax Class. T.D: DeMeo Tax Class.

Ref: S = SiMDA, C = Carry (2012)

Diameter estimates

DesignationDiameter / Err (km)ΔD/DMethodYearRefNχ2Use
(762) Pulcova137.08 ± 3.202.3 % STM2004D93 0.10 1
(762) Pulcova143.00 ± 2.001.4 % NEATM2008D47 6.00 2
(762) Pulcova118.70 ± 3.302.8 % STM2010D642 34.56 3
(762) Pulcova147.76 ± 8.355.7 % NEATM2010D64 1.34 4
(762) Pulcova129.21 ± 1.781.4 % STM2011D832 24.95 5
(762) Pulcova141.72 ± 1.531.1 % NEATM2011D72 5.60 6

plot, average diameter and derived density

All

Notes (N):
1: This estimate is discarded for the average diameter (and derived density) calculation in Carry (2012).
2: This estimate is discarded for the average diameter (and derived density) calculation in SiMDA (catalog).

NEATM : Near-Earth Asteroid Thermal Model. STM : Standard Thermal Model.


EVM diam. average D = (138.1 ± 7.58) km   (ΔD/D = 5%, SNR = 18.22) Derived bulk density ρ = (1.17 ± 1.78) g/cm3   (Δρ/ρ = 152%, SNR = 0.7)


References
D47(2008):Marchis, F., Descamps, P., Baek, M., Harris, A.W., Kaasalainen, M., Berthier, J., Hestroffer, D., Vachier, F., 2008. Main belt binary asteroidal systems with circular mutual orbits. Icarus 196, 97–118.
D64(2010):Ryan, E.L., Woodward, C.E., 2010. Rectified Asteroid Albedos and Diameters from IRAS and MSX Photometry Catalogs. Astronomical Journal 140, 933–943.
D72(2011):Masiero, J.R., Mainzer, A.K., Grav, T., Bauer, J.M., Cutri, R.M., Dailey, J., Eisenhardt, P.R.M., McMillan, R.S., Spahr, T.B., Skrutskie, M.F., Tholen, D., Walker, R.G., Wright, E.L., DeBaun, E., Elsbury, D., Gautier, IV, T., Gomillion, S., Wilkins, A., 2011. Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters. Astrophysical Journal 741, 68.
D83(2011):Usui, F., Kuroda, D., Müller, T.G., Hasegawa, S., Ishiguro, M., Ootsubo, T., Ishihara, D., Kataza, H., Takita, S., Oyabu, S., Ueno, M., Matsuhara, H., Onaka, T., 2011. Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey. Publications of the Astronomical Society of Japan 63, 1117–1138.
D93(2004):Tedesco, E.F., Noah, P.V., Noah, M.C., Price, S.D., 2004. IRAS Minor Planet Survey. NASA Planetary Data System. IRAS-A-FPA-3-RDR-IMPS-V6.0.

Mass estimates

DesignationMass / Err (kg)ΔM/MMethodYearRefNχ2Use
(762) Pulcova2.59e+18 ± 3.98e+1715 %BinImg 2002M32125.98 1
(762) Pulcova1.40e+18 ± 9.94e+167 %BinImg 2008M754.76 2
(762) Pulcova1.25e+19 ± 7.46e+1860 %Deflec 2011M97122.13 3
(762) Pulcova3.15e+19 ± 7.45e+1824 %Deflec 2011M971216.09 4
(762) Pulcova1.11e+18 ± 4.42e+1740 %Ephem 2011M10011.32 5
(762) Pulcova9.01e+17 ± 4.47e+1750 %Ephem 2019M1262.56 6

plot, average mass and derived density

All

Notes (N):
1: This estimate is discarded for the average mass (and derived density) calculation in Carry (2012).
2: This estimate is discarded for the average mass (and derived density) calculation in SiMDA (catalog).
3: This estimate is an average of individual solutions listed before under the same reference (e.g. M125).

BinImg : Binary imaged at optical wavelength. Deflec : Orbital deflection (close encounter) of one or several test asteroids (classical LSQ). Ephem : Planetary ephemeris solution.


EVM mass average M = (1.617 ± 2.440) × 1018 kg   (ΔM/M = 151%, SNR = 0.7) Derived bulk density ρ = (1.17 ± 1.78) g/cm3   (Δρ/ρ = 152%, SNR = 0.7)


References
M32(2002):Merline, W.J., Weidenschilling, S.J., Durda, D.D., Margot, J.L., Pravec, P., Storrs, A.D., 2002. Asteroids Do Have Satellites. Asteroids III , 289–312.
M75(2008):Marchis, F., Descamps, P., Baek, M., Harris, A.W., Kaasalainen, M., Berthier, J., Hestroffer, D., Vachier, F., 2008a. Main belt binary asteroidal systems with circular mutual orbits. Icarus 196, 97–118.
M97(2011):Zielenbach, W., 2011. Mass Determination Studies of 104 Large Asteroids. Astronomical Journal 142, 120–128.
M100(2011):Fienga, A., Kuchynka, P., Laskar, J., Manche, H., Gastineau, M., 2011. Asteroid mass determinations with INPOP planetary ephemerides. EPSC-DPS Joint Meeting 2011 , 1879.
M126(2019):Fienga, A., et. al, 2019. INPOP19a planetary ephemeris. Notes Scientifiques et Techniques de l'Institut de mécanique céleste,