3 Puppis

Short description: Binary star system in the constellation Puppis

3 Puppis

Location of 3 Puppis (circled)

Observation data
Equinox J2000.0]] (ICRS)
Constellation | Puppis
Right ascension |  07h 43m 48.46872s[1]
Declination | −28° 57′ 17.3720″[1]
Apparent magnitude (V) | 3.93[2]
Characteristics
Spectral type | A2.7Ib[2] (A2Ia - A3IIpe[3])
Apparent magnitude (K) | 2.340[4]
U−B color index | −0.09[5]
B−V color index | +0.18[5]
Astrometry
Radial velocity (Rv)| 4.95±0.10[6] km/s
Proper motion (μ)|  RA: −5.09[1] mas/yr
Dec.: +3.90[1] mas/yr
Parallax (π)| 0.59 ± 0.17[1] mas
Distance| 2,100±280 ly
(630±85 pc)
Absolute magnitude (MV)| −5.5[2]
Orbit[6]
Primary| A
Companion| B
Period (P)| 137.52±0.04 days
Semi-major axis (a)| 1.11±0.03 astronomical unit|AU[7]
Eccentricity (e)| 0
Periastron epoch (T)| 56,725.5±0.9
Semi-amplitude (K1)
(primary)| 4.75±0.15 km/s
Details[7]

Mass| 8.8±0.5 M☉
Radius| 54±7 R☉
Luminosity| 12,600+3,300
−2,600 L☉
Surface gravity (log g)| 1.9±0.1 cgs
Temperature| 8,500±500 K
Rotational velocity (v sin i)| 35±5 km/s

Mass| 0.75±0.25 M☉
Radius| 0.3 R☉
Surface gravity (log g)| 5.0 cgs
Temperature| 50,000 K
Other designations

l Puppis, GSC 06552-03228, HD 62623, HIP 37677, HR 2996, SAO 174400, CD−28°4774

Database references
SIMBAD| data

3 Puppis (3 Pup) is a spectroscopic binary in the constellation Puppis. It is a very rare A[e] supergiant, referred to as a B[e] star despite its spectral classification, and its apparent magnitude is 3.93.

3 Puppis is surrounded by a disc of circumstellar dust, which is unusual for an A-type star.[3] It is caused by a low mass companion, a helium-rich subdwarf that is transferring mass to the supergiant. Due to mass transfer, its mass reduced from 3.6 M☉ when it formed to the current 0.75 M☉.[7] Like most B[e] stars, 3 Pup rotates rapidly, at 20%[lower-alpha 1] of the speed at which it would start to break apart. The disc has its inner edge only 3.8 AU from the primary star and it is suspected that deceleration of the hot primary stellar wind by the companion allows the dust to form unusually close to such a luminous star.[3]

## Notes

1. ↑ Calculated from rotational velocity divided by critical velocity, 35/178 = 0.20.

## References

1. ↑ 1.0 1.1 1.2 1.3 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.
2. ↑ 2.0 2.1 2.2 Klochkova, V. G.; Sendzikas, E. G.; Chentsov, E. L. (2015). "Spectral atlas of A-type supergiants". Astrophysical Bulletin 70 (1): 99–108. doi:10.1134/S1990341315010113. Bibcode: 2015AstBu..70...99K.
3. ↑ 3.0 3.1 3.2 Meilland, A.; Kanaan, S.; Borges Fernandes, M.; Chesneau, O.; Millour, F.; Stee, Ph.; Lopez, B. (2010). "Resolving the dusty circumstellar environment of the A[e] supergiant HD 62623 with the VLTI/MIDI". Astronomy and Astrophysics 512: A73. doi:10.1051/0004-6361/200913640. Bibcode: 2010A&A...512A..73M.
4. ↑ Kraus, M.; Oksala, M. E.; Cidale, L. S.; Arias, M. L.; Torres, A. F.; Borges Fernandes, M. (2015). "Discovery of SiO Band Emission from Galactic B[e] Supergiants". The Astrophysical Journal Letters 800 (2): L20. doi:10.1088/2041-8205/800/2/L20. Bibcode: 2015ApJ...800L..20K.
5. ↑ 5.0 5.1 Gutierrez-Moreno, A.; Moreno, H.; Loyola, P.; Cortes, G. (1986). "Low dispersion spectrophotometry of bright early-type stars". Astronomy and Astrophysics Supplement Series 64: 205. Bibcode: 1986A&AS...64..205G.
6. ↑ 6.0 6.1 Vaidman, Nadezhda L.; Nurmakhametova, Shakhida T.; Miroshnichenko, Anatoly S.; Khokhlov, Serik A.; Agishev, Aldiyar T.; Khokhlov, Azamat A.; Ashimov, Yeskendyr K.; Yermekbayev, Berik S. (2025-09-02). "Determination of Orbital Parameters of Binary Star Systems Using the MCMC Method" (in en). Galaxies 13 (5): 101. doi:10.3390/galaxies13050101. ISSN 2075-4434. Bibcode: 2025Galax..13..101V.
7. ↑ 7.0 7.1 7.2 Miroshnichenko, A. S.; Danford, S.; Zharikov, S. V.; Klochkova, V. G.; Chentsov, E. L.; Vanbeveren, D.; Zakhozhay, O. V.; Manset, N. et al. (July 2020). "Properties of Galactic B[e] Supergiants. V. 3 Pup–Constraining the Orbital Parameters and Modeling the Circumstellar Environments" (in en). The Astrophysical Journal 897 (1): 48. doi:10.3847/1538-4357/ab93d9. ISSN 0004-637X. Bibcode: 2020ApJ...897...48M.

* v
* t
* e

Stars of Puppis

Bayer|

* ζ (Naos)
* ν
* ξ (Azmidi)
* ο
* π
* ρ (Tureis)
* σ
* τ
* χ
* L2

Flamsteed|

* 1
* 2
* 3 (l)
* 4
* 5
* 6
* 8
* 9
* 10
* 11 (j)
* 12
* 14
* 16
* 18
* 19
* 20
* 21
* 22

Variable|

* R
* T (not variable)
* V
* Z
* RS
* RX
* ST
* TY
* UY
* UZ
* VV
* VX
* VZ
* WW
* AQ
* AR
* AU
* BB
* BN
* BV
* CP
* HH
* HZ
* KQ
* MX (r)
* MY (y3)
* MZ
* NO
* NP
* NS (h1)
* NV (υ1)
* NW (υ2)
* NX
* OU (L1)
* OS
* OW (z)
* OX
* PQ
* PR
* PT
* PU (m)
* PV
* PX
* PY
* QS
* QU
* QW (I)
* QY
* QZ (b)
* V336
* V338
* V339
* V347
* V348
* V351
* V363
* V368
* V376
* V378
* V390
* V392
* V397
* V420
* V436
* V438
* V443
* V445
* V468 (d4)
* V510
* V574
* V575
* V596
* V597
* V598

HR|

* 2157
* 2158
* 2178
* 2187
* 2204
* 2211
* 2348 (G)
* 2384
* 2462 (V)
* 2475
* 2482
* 2488
* 2518 (x)
* 2548 (X)
* 2549
* 2558
* 2563
* 2579
* 2594
* 2604
* 2608
* 2612
* 2619 (t)
* 2626
* 2641
* 2658
* 2666 (C)
* 2667
* 2672 (H)
* 2677
* 2685
* 2687
* 2691 (D)
* 2702 (A)
* 2719
* 2727 (E)
* 2759
* 2762
* 2769
* 2770
* 2771
* 2789 (M)
* 2791 (F)
* 2794
* 2829
* 2856
* 2860
* 2863
* 2868
* 2870
* 2873
* 2874
* 2875 (y)
* 2881
* 2895
* 2897
* 2899
* 2900
* 2906
* 2909 (n)
* 2910 (n)
* 2913
* 2916
* 2922 (p)
* 2923
* 2933
* 2937 (f)
* 2940 (y2)
* 2945
* 2948 (k1)
* 2949 (k2)
* 2954 (e)
* 2955
* 2956
* 2959
* 2960
* 2961 (d1)
* 2963 (d2)
* 2964 (d3)
* 2976
* 2981
* 2984
* 2988
* 2994
* 2998
* 3001
* 3002 (W)
* 3007
* 3011
* 3017 (c)
* 3018
* 3019
* 3020
* 3023
* 3027
* 3035
* 3037
* 3042
* 3043
* 3046 (Q)
* 3051
* 3052
* 3055 (P)
* 3057
* 3060
* 3068
* 3069
* 3071
* 3074
* 3079
* 3080 (a)
* 3085
* 3089
* 3090 (J)
* 3091
* 3092
* 3096
* 3101
* 3111
* 3114
* 3116 (N)
* 3118
* 3121 (O)
* 3131
* 3137
* 3140
* 3142
* 3143
* 3148
* 3154
* 3155
* 3160
* 3166
* 3177
* 3183
* 3190
* 3194
* 3199
* 3205
* 3219
* 3226
* 3233
* 3238
* 3239
* 3241
* 3242
* 3243 (h2)
* 3251
* 3253
* 3259
* 3261
* 3266
* 3270 (q)
* 3273
* 3276
* 3279
* 3281
* 3282 (w)
* 3283
* 3286
* 3291
* 3308
* 3315
* 3316
* 3317
* 3320
* 3324
* 3326

HD|

* 44594
* 48265 (Nosaxa)
* 49798
* 50499
* 53680
* 53706
* 59235
* 61005
* 61589
* 61750
* 62542
* 63291
* 63399
* 63696
* 63734
* 65638
* 66885
* 67408
* 69904
* 70642

Gliese|

* Gliese 257
* Gliese 283
* Gliese 300

Other|

* 171 G. Puppis
* Bran 76
* L 745-46A
* 2MASS 0729−39
* NGC 2423-3
* OH 231.8+4.2
* PSR B0740−28
* PSR B0808−13
* PSR J0737−3039
* PSR J0738−4042
* RX J0812.4−3114
* RX J0822−4300
* SCR J0740−4257
* SWIFT J0732.5−1331
* 4U 0728-25
* WASP-121

* List

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