Rho Puppis

Short description: Star in the southern constellation of Puppis

Not to be confused with R Puppis.

"Tureis" redirects here. For the other star traditionally named Tureis, see Iota Carinae.

ρ Puppis

Location of ρ Puppis (circled)

Observation data
Equinox J2000.0]] (ICRS)
Constellation | Puppis
Right ascension |  08h 07m 32.64882s[1]
Declination | −24° 18′ 15.5679″[1]
Apparent magnitude (V) | 2.78[2] (2.68 - 2.87)[3]
Characteristics
Spectral type | F5IIkF2IImF5II[4]
U−B color index | +0.17[2]
B−V color index | +0.40[2]
Variable type | δ Sct[5]
Astrometry
Radial velocity (Rv)| +46.1[6] km/s
Proper motion (μ)|  RA: –83.35[1] mas/yr
Dec.: +46.23[1] mas/yr
Parallax (π)| 51.33 ± 0.15[1] mas
Distance| 63.5 ± 0.2 ly
(19.48 ± 0.06 pc)
Absolute magnitude (MV)| 1.41[7]
Details
Mass| 1.5±0.1[8] M☉
Radius| 3.52±0.07[8] R☉
Luminosity| 24.0±0.2[9] L☉
Surface gravity (log g)| 3.58±0.14[9] cgs
Temperature| 6,650±100[9] K
Metallicity [Fe/H]| 0.35[10] dex
Rotational velocity (v sin i)| 13±1[9] km/s
Age| 2[11] Gyr
Other designations

ρ Puppis, 15 Puppis, CPD−23°3368, FK5 308, HD 67523, HIP 39757, HR 3185, SAO 175217[12]

Database references
SIMBAD| data

Rho Puppis (ρ Puppis, abbreviated Rho Pup, ρ Pup), formally named Tureis /ˈtjʊəreɪs/,[13] is a star in the southern constellation of Puppis. With an average apparent visual magnitude of 2.78,[2] it is the third-brightest member of this generally faint constellation. Based upon parallax measurements made during the Hipparcos mission, Rho Puppis is located at a distance of 63.5 light-years (19.5 parsecs) from the Sun.[1] It is the prototype of the Rho Puppis class of evolved Am stars.

## Nomenclature

ρ Puppis (Latinised to Rho Puppis) is the star's Bayer designation.

It bore the traditional name Tureis or Turais, from the Arabic تُرَيْس turays "shield" (diminutive), which was shared by Iota Carinae.[14] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[15] to catalogue and standardize proper names for stars. The WGSN approved the name Tureis for this star on 12 September 2016 and it is now so entered in the IAU Catalog of Star Names (Iota Carinae was given the name Aspidiske on 20 July 2016).[13]

## Properties

A light curve for Rho Puppis, plotted from TESS data[16]

At present Rho Puppis is moving away from the Sun with a radial velocity of +46.1 km s−1. The closest approach occurred about 394,000 years ago when it came within roughly 11.6 ly (3.6 pc) of the Solar System; about the same distance as Procyon in the present era.[17]

The variability of this star was announced in 1956 by American astronomer Olin J. Eggen.[5] It was determined to be a Delta Scuti-type variable star, making it one of the first stars of that type to be identified. Photometric observations dating back to 1946 provide a lengthy record of its pattern of pulsation; it undergoes periodic pulsations with a single period of 0.14088143(3) days,[18] or 7.1 cycles per day. During each cycle, the star's magnitude varies with an amplitude of 0.15 and the radial velocity varies by 10 km s−1. The peak brightness occurs 28.8 minutes following the minimum radial velocity.[5] The outer atmosphere's effective temperature of 6,650 K[9] is one of the lowest known for a Delta Scuti variable.[5] In 2017, a magnetic field was discovered around Rho Puppis, making it the second Delta Scuti star known to have a magnetic field, after HD 188774.[19]

Rho Puppis has an estimated age of about 2 billion years[11] and it has 3.52 times the Sun's radius.[8] It has a stellar classification of F5IIkF2IImF5II.[4] This complex format indicates that ρ Puppis is an Am star, with relatively weak lines of calcium and strong lines of other metals. The spectral type indicated by the calcium k line is F5, while that indicated by heavier metal absorption lines is F2. The roman numerals indicate a luminosity class of bright giant. Most such stars are found in binary star systems,[20] but this appears to be an exception as no companion has been discovered.[11][21] Evolved stars with Am-like peculiarities of abundance have come to be known as ρ Puppis stars.[22] The star's metallicity is more than double that in the Sun.[10]

This star shows an excess emission of infrared radiation, suggesting that there is a circumstellar disk of dust orbiting this star. The mean temperature of the emission is 85 K, corresponding to an orbital separation from the host star of 50 AU.[23][11]

## References

1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 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 2.3 Bookmeyer, B. B. et al. (August 1977), "Photoelectric UBV observations of RR Lyrae variable stars. Second list", Revista Mexicana de Astronomía y Astrofísica 2: 235–258, Bibcode: 1977RMxAA...2..235B
3. ↑ Samus', N. N et al. (2017), "General catalogue of variable stars", Astronomy Reports, GCVS 5.1 61 (1): 80, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S
4. ↑ 4.0 4.1 Gray, R. O; Corbally, C. J; Garrison, R. F; McFadden, M. T; Robinson, P. E (2003), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I", The Astronomical Journal 126 (4): 2048, doi:10.1086/378365, Bibcode: 2003AJ....126.2048G
5. ↑ 5.0 5.1 5.2 5.3 Mathias, P. et al. (November 1997), "A spectroscopic study of the delta Scuti star rho Puppis", Astronomy and Astrophysics 327: 1077–1086, Bibcode: 1997A&A...327.1077M
6. ↑ Evans, D. S. (June 20–24, 1966), Batten, Alan Henry; Heard, John Frederick, eds., "The Revision of the General Catalogue of Radial Velocities", Determination of Radial Velocities and Their Applications, Proceedings from IAU Symposium No. 30 (University of Toronto: International Astronomical Union) 30: 57, Bibcode: 1967IAUS...30...57E
7. ↑ Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics 542: A116, doi:10.1051/0004-6361/201118724, Bibcode: 2012A&A...542A.116A
8. ↑ 8.0 8.1 8.2 Antoci, V.; Handler, G.; Grundahl, F.; Carrier, F.; Brugamyer, E. J.; Robertson, P.; Kjeldsen, H.; Kok, Y. et al. (2013-10-21), "Searching for solar-like oscillations in the δ Scuti star ρ Puppis" (in en), Monthly Notices of the Royal Astronomical Society 435 (2): 1563–1575, doi:10.1093/mnras/stt1397, ISSN 1365-2966
9. ↑ 9.0 9.1 9.2 9.3 9.4 Nardetto, N.; Poretti, E.; Rainer, M.; Guiglion, G.; Scardia, M.; Schmid, V. S.; Mathias, P. (2014-01-01), "Understanding the dynamical structure of pulsating stars - HARPS spectroscopy of the δ Scuti stars ρ Puppis and DX Ceti" (in en), Astronomy & Astrophysics 561: A151, doi:10.1051/0004-6361/201322356, ISSN 0004-6361, Bibcode: 2014A&A...561A.151N
10. ↑ 10.0 10.1 Burkhart, C.; Coupry, M. F. (September 1991), "The A and Am-Fm stars. I - The abundances of Li, Al, Si, and Fe", Astronomy and Astrophysics 249 (1): 205–216, Bibcode: 1991A&A...249..205B
11. ↑ 11.0 11.1 11.2 11.3 Rodriguez, David R.; Zuckerman, B. (February 2012), "Binaries among Debris Disk Stars", The Astrophysical Journal 745 (2): 147, doi:10.1088/0004-637X/745/2/147, Bibcode: 2012ApJ...745..147R
12. ↑ "rho Pup". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=rho+Pup.
13. ↑ 13.0 13.1 IAU Catalog of Star Names, http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt, retrieved 28 July 2016
14. ↑ Moore, Patrick (2005), The observer's year: 366 nights of the universe, Practical Astronomy (2nd ed.), Springer, p. 346, ISBN 1-85233-884-9, https://books.google.com/books?id=0Pu_YNynaiYC&pg=PA346
15. ↑ IAU Working Group on Star Names (WGSN), International Astronomical Union, https://www.iau.org/science/scientific_bodies/working_groups/280/, retrieved 22 May 2016
16. ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html, retrieved 4 September 2022
17. ↑ García-Sánchez, J. et al. (November 2001), "Stellar encounters with the solar system", Astronomy and Astrophysics 379 (2): 634–659, doi:10.1051/0004-6361:20011330, Bibcode: 2001A&A...379..634G
18. ↑ Moon, T.; van Antwerpen, C. (June 2009), "Period Changes in δ Scuti Stars: ρ Puppis", The Journal of the American Association of Variable Star Observers 37 (1): 3–14, Bibcode: 2009JAVSO..37....3M
19. ↑ Neiner, C.; Wade, G. A.; Sikora, J. (2017-06-11). "Discovery of a magnetic field in the δ Scuti F2m star ρ Pup" (in en). Monthly Notices of the Royal Astronomical Society: Letters 468 (1): L46–L49. doi:10.1093/mnrasl/slx023. ISSN 1745-3925. Bibcode: 2017MNRAS.468L..46N. https://academic.oup.com/mnrasl/article/468/1/L46/2972865.
20. ↑ Netopil, M. et al. (November 2008), "Chemically peculiar stars and their temperature calibration", Astronomy and Astrophysics 491 (2): 545–554, doi:10.1051/0004-6361:200810325, Bibcode: 2008A&A...491..545N
21. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869–879, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E
22. ↑ Neiner, C; Wade, G. A; Sikora, J (2017), "Discovery of a magnetic field in the δ Scuti F2m star ρ Pup", Monthly Notices of the Royal Astronomical Society: Letters 468 (1): L46–L49, doi:10.1093/mnrasl/slx023, Bibcode: 2017MNRAS.468L..46N
23. ↑ Rhee, Joseph H. et al. (May 2007), "Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs", The Astrophysical Journal 660 (2): 1556–1571, doi:10.1086/509912, Bibcode: 2007ApJ...660.1556R

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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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