TX Piscium

TX Piscium (19 Piscium) is a variable carbon star in the constellation Pisces. It is amongst the reddest naked eye stars, with a significant reddish hue when seen in binoculars. It is approximately 900 light years from Earth.

TX Piscium
Location of TX Piscium (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Pisces
Right ascension  23h 46m 23.51708s[1]
Declination +03° 29′ 12.5244″[1]
Apparent magnitude (V) 4.79 - 5.20[2]
Characteristics
Spectral type C7,2[3]
U−B color index +3.33[4]
B−V color index +2.60[4]
Variable type Lb[2]
Astrometry
Radial velocity (Rv)+11.5±1.5[5] km/s
Proper motion (μ) RA: −33.68[1] mas/yr
Dec.: −24.49[1] mas/yr
Parallax (π)3.63 ± 0.39[1] mas
Distanceapprox. 900 ly
(approx. 280 pc)
Absolute magnitude (MV)−2.22[5]
Details
Mass1 - 3[6] M☉
Radius295[6] R☉
Luminosity7,019 - 7,876[6] L☉
Surface gravity (log g)−0.2 - −0.5[6] cgs
Temperature3,080 - 3,170[6] K
Metallicity [Fe/H]−0.39[7] dex
Other designations
19 Psc, TX Psc, BD+02° 4709, FK5 3908, HD 223075, HIP 117245, HR 9004, SAO 128374
Database references
SIMBADdata

Spectrum

TX Piscium is a very red star, 2.6 magnitudes fainter at blue wavelengths than in the middle of the visual range, and another 3.3 magnitudes fainter in the ultraviolet.[4]

It has been given a spectral class C7,2, indicating a relatively cool carbon star with only modest C2 band strength.[3] It has alternately been classified as C-N5 C24, suggesting a warmer star with stronger C2 bands.[8] Spectral features have been observed to vary.[9]

Variability

The apparent magnitude of TX Piscium varies between +4.9 and +5.5 and it is classified as a slow irregular variable.[2] Photometry has shown some periodicity in the brightness of 224 days, and some spectral variation over 450 days, suggesting the star is not entirely irregular.[9]

The star apparently lies on the period-luminosity relation corresponding to fundamental mode pulsations, unusual for a low-amplitude semi-regular or irregular variable which usually pulsate in an overtone.[10] The angular diameter has been measured at around 10 mas, although this varies depending on the observed wavelength and the atmosphere appears to be highly asymmetric. There may be one or more "blobs" of ejected material near the star.[10][9] Some observations show the angular diameter to change in synchrony with the visual brightness.[10]

Properties

TX Piscium is a thermally-pulsing asymptotic giant branch (TP-AGB) star, which means that it is alternately fusing helium in a shell around its core and fusing hydrogen in a shell closer to its surface. Stars on the TP-AGB are generally unstable, with high mass loss and pulsations.

The periodic flashes of the helium shell in a TP-AGB star are known as thermal pulses and cause the hydrogen shell to be extinguished. This creates strong convection and the third dredge-up (TDU) which brings helium fusion products such as carbon to the surface. After several TDUs, the abundance of carbon in the atmosphere begins to exceed that of oxygen and then the star is known as a carbon star. In TX Piscium, the carbon/oxygen ratio is calculated to be 1.03, which is at the low end of the scale of carbon stars.[7] It is thought to be a relatively new carbon star.[9]

TX Piscium has a mass of approximately 2 M☉. Modelling of its observed properties suggest a mass between 1 and 2 M☉, while evolutionary models suggest a mass between 2 and 3 M☉. In particular, stars with a mass below 2 M☉ are not expected to become carbon stars.[6]

The temperature of TX Piscium is thought to vary between 3,080 K at minimum visual brightness and 3,170 K at visual maximum. Similarly, its luminosity varies between 7,019 and 7876 L☉. Many of its physical properties are uncertain due to uncertainty in its distance. The Hipparcos parallax corresponds to a distance of 275 parsecs, but other estimates give distances as high as 315 parsecs.[6]

gollark: Yes.
gollark: ubq, or something? Troubling.
gollark: Palaiologos appears to have repeatedly denied transparency in various ways, I think talking about "different kinds" of transparency and then just denying that it was a good thing.
gollark: This is an increase in transparency.
gollark: I don't consider any of the staff's operation transparent, since everything gets done over backchannels and then hidden as, apparently, "unnecessary details".

References
  1. Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
  2. Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. Yamashita, Yasumasa (1972), "The C-classification of the spectra of carbon stars", Annals of the Tokyo Astronomical Observatory, 13 (3), Bibcode:1972AnTok..13..169Y
  4. Ducati, J. R (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  5. Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.
  6. Klotz, D; Paladini, C; Hron, J; Aringer, B; Sacuto, S; Marigo, P; Verhoelst, T (2013). "Catching the fish – Constraining stellar parameters for TX Piscium using spectro-interferometric observations". Astronomy & Astrophysics. 550: A86. arXiv:1301.0404. Bibcode:2013A&A...550A..86K. doi:10.1051/0004-6361/201220444.
  7. Abia, C; Cunha, K; Cristallo, S; De Laverny, P (2015). "The origin of fluorine: Abundances in AGB carbon stars revisited". Astronomy & Astrophysics. 581: A88. arXiv:1507.03488. Bibcode:2015A&A...581A..88A. doi:10.1051/0004-6361/201526586.
  8. Barnbaum, Cecilia; Stone, Remington P. S; Keenan, Philip C (1996). "A Moderate-Resolution Spectral Atlas of Carbon Stars: R, J, N, CH, and Barium Stars". The Astrophysical Journal Supplement Series. 105: 419. Bibcode:1996ApJS..105..419B. doi:10.1086/192323.
  9. Hron, J; Uttenthaler, S; Aringer, B; Klotz, D; Lebzelter, T; Paladini, C; Wiedemann, G (2015). "The complex environment of the bright carbon star TX Piscium as probed by spectro-astrometry". Astronomy & Astrophysics. 584: A27. arXiv:1510.02680. Bibcode:2015A&A...584A..27H. doi:10.1051/0004-6361/201526862.
  10. Cruzalèbes, P; Jorissen, A; Rabbia, Y; Sacuto, S; Chiavassa, A; Pasquato, E; Plez, B; Eriksson, K; Spang, A; Chesneau, O (2013). "Fundamental parameters of 16 late-type stars derived from their angular diameter measured with VLTI/AMBER★". Monthly Notices of the Royal Astronomical Society. 434: 437. arXiv:1306.3288. Bibcode:2013MNRAS.434..437C. doi:10.1093/mnras/stt1037.
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