55 Cancri

55 Cancri
Diagram showing star positions and boundaries of the constellation of Cancer and its surroundings


A star chart of the constellation of Cancer showing the position of 55 Cancri (circled)

Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cancer
55 Cancri A
Right ascension 08h 52m 35.81s[1]
Declination +28° 19′ 51.0″[1]
Apparent magnitude (V) 5.95
55 Cancri B
Right ascension 08h 52m 40.9s
Declination +28° 19′ 59″
Apparent magnitude (V) 13.15
Characteristics
Spectral type G8V / M3.5-4V
U−B color index 0.65 / 1.66
B−V color index 0.86 / 1.21
Astrometry
Radial velocity (Rv)27.3 km/s
Proper motion (μ) RA: -485.80 ± 0.97[1] mas/yr
Dec.: -234.05 ± 0.68[1] mas/yr
Parallax (π)81.03 ± 0.75[1] mas
Distance40.3 ± 0.4 ly
(12.3 ± 0.1 pc)
Absolute magnitude (MV)5.46 / 12.66
Details
Mass0.95 ± 0.1 / 0.13 M☉
Radius1.152 ± 0.035 [2] / 0.30 R☉
Luminosity0.57 ± 0.01[3] L☉
Luminosity (bolometric)0.63 / 0.0076 L☉
Temperature5373 ± 9.7 [4] K
Metallicity [Fe/H]+0.27[5] dex
Rotation42.2 d
Age(7.4–8.7) × 109[6] years
Other designations
Copernicus, HR 3522, BD+28°1660, Gliese 324, HD 75732, HIP 43587, Rho1 Cancri
Database references
SIMBADdata
Exoplanet Archivedata
ARICNSdata
Extrasolar Planets
Encyclopaedia		data

55 Cancri (/ˈkæŋkraɪ/ or /ˈkæŋkriː/) (abbreviated 55 Cnc) is a binary star approximately 41 light-years away from the Sun in the constellation of Cancer. The system consists of a G-type star (designated 55 Cancri A, also named Copernicus[7]) and a smaller red dwarf (55 Cancri B).

As of 2015, five extrasolar planets (designated 55 Cancri b, c, d, e and f; named Galileo, Brahe, Lipperhey, Janssen and Harriot, respectively) are believed to orbit 55 Cancri A.

Nomenclature

55 Cancri is the system's Flamsteed designation. It also bears the Bayer designation ρ¹ Cancri (Latinised to Rho¹ Cancri) and the Bright Star Catalogue designation HR 3522. The two components are designated A and B,[8] though A is itself sometimes referred to as 55 Cancri.[5] The first planet discovered orbiting 55 Cancri A was designated HR 3522b by its discoverers,[9] though it is more commonly referred to as 55 Cancri b.[10] Under the rules for naming objects in binary star systems it should be named 55 Cancri Ab[11] and this more formal form is occasionally used to avoid confusion with the secondary star 55 Cancri B. The other planets discovered were designated 55 Cancri c, d, e and f, in order of their discovery.

In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars.[12] The process involved public nomination and voting for the new names.[13] In December 2015, the IAU announced the winning names were Copernicus for 55 Cancri A and Galileo, Brahe, Lipperhey, Janssen and Harriot for its planets (b, c, d, e and f, respectively).[14]

The winning names were those submitted by the Royal Netherlands Association for Meteorology and Astronomy of the Netherlands. They honor the astronomers Nicolaus Copernicus, Galileo Galilei, Tycho Brahe and Thomas Harriot and the spectacle makers and telescope pioneers Hans Lipperhey and Jacharias Janssen.[15] (The IAU originally announced the winning name was Lippershey for 55 Cancri d. In January 2016, in recognition that his actual name was Lipperhey (with Lippershey an error introduced in the 19th century), the exoplanet name was corrected to Lipperhey by the IAU and that name was submitted to the official sites that keep track of astronomical information.[14][15])

In 2016, the IAU organized a Working Group on Star Names (WGSN)[16] to catalog and standardize proper names for stars. In its first bulletin of July 2016,[17] the WGSN explicitly recognized the names of exoplanets and their host stars approved by the Executive Committee Working Group Public Naming of Planets and Planetary Satellites, including the names of stars adopted during the 2015 NameExoWorlds campaign. This star is now so entered in the IAU Catalog of Star Names.[7]

Stellar system

The 55 Cancri system is located fairly close to the Solar System: the Hipparcos astrometry satellite measured the parallax of 55 Cancri A as 81.03 milliarcseconds, corresponding to a distance of 12.3 parsecs (40.3 light years).[1] 55 Cancri A has an apparent magnitude of 5.95, making it just visible to the naked eye under very dark skies. The red dwarf 55 Cancri B is of the 13th magnitude and only visible through a telescope. The two components are separated by an estimated distance of 1065 AU[18] (one thousand times the distance from the Earth to the Sun). Despite their wide separation, the two stars appear to be gravitationally bound, as they share a common proper motion.[5]

The primary star, 55 Cancri A, is a yellow dwarf star of main sequence spectral type G8V. It is smaller in radius and slightly less massive than the Sun, and so is cooler and less luminous. The star has only low emission from its chromosphere, and is not variable in the visible spectrum;[5] but it is variable in X-rays.[19] It is more enriched than the Sun in elements heavier than helium, with 186% the solar abundance of iron; it is therefore classified as a rare "super metal-rich" (SMR) star.[5] This abundance of metal makes estimating the star's age and mass difficult, as evolutionary models are less well defined for such stars. Age estimates for 55 Cancri A include 7.4-8.7 billion years[6] and 10.2 ± 2.5 billion years.[20]

A hypothesis for the high metal content in SMR dwarf stars is that material enriched in heavy elements fell into the atmosphere from a protoplanetary disk. This would pollute the star's external layers, resulting in a higher than normal metallicity. The lack of a deep convection zone would mean that the outer layers would retain higher abundance ratios of these heavy elements.[21]

Observations of 55 Cancri A in the submillimeter region of the spectrum have thus far failed to detect any associated dust. The upper limit on emissions within 100 AU of this star is about 850 mJy, at a wavelength of 850 μm. This limits the total mass of fine dust around the star to less than 0.01% of the Earth's mass. However, this does not exclude the presence of an asteroid belt or a Kuiper belt equivalent.[22]

The secondary, 55 Cancri B, is a red dwarf star much less massive and luminous than the Sun. There are indications that component B may itself be a double star, though this is uncertain.[8]

Planetary system

Comparison of the orbits of the inner planets of 55 Cancri A (black) with the planets of the Solar System.

The 55 Cancri system was the first known to have four, and later five planets, and may possibly have more. The innermost planet, e, transits 55 Cancri A as viewed from Earth.[23] The next planet, b, is non-transiting but there is tentative evidence that it is surrounded by an extended atmosphere that does transit the star.[19]

In 1997, the discovery of a 51 Pegasi-like planet orbiting 55 Cancri A was announced, together with the planet of Tau Boötis and the inner planet of Upsilon Andromedae.[9] The planet was discovered by measuring the star's radial velocity, which showed a periodicity of around 14.7 days corresponding to a planet at least 78% of the mass of Jupiter. These radial velocity measurements still showed a drift unaccounted-for by this planet, which could be explained by the gravitational influence of a more distant object.

In 1998 the discovery of a possible dust disk around 55 Cancri A was announced.[24] Calculations gave the disk radius at least 40 AU, similar to the Kuiper belt in the Solar System, with an inclination of 25° with respect to the plane of the sky. However, the discovery could not be verified and was later deemed to be spurious, caused instead by background galaxies.[25]

The Solar system compared with the planetary system of 55 Cancri. (Note: this depiction was made before planets e and f were discovered.)

After making further radial velocity measurements, a planet orbiting at a distance of around 5 AU was announced in 2002.[5] This planet received the designation 55 Cancri d. At the time of discovery, the planet was thought to be in an orbit of mild eccentricity (close to 0.1), but this value was increased by later measurements. Even after accounting for these two planets, a periodicity at 43 days remained, possibly due to a third planet. Measurements of the star suggested that this was close to the star's rotation period, which raised the possibility that the 43-day signal was caused by stellar activity. This possible planet received the designation 55 Cancri c.

Artist's Rendition of 55 Cnc's planets

55 Cancri e was announced in 2004.[26] With 8.3 Earth masses, it is a large super-Earth which was originally thought to have an orbital period of 2.8 days, though it was later found that this was an alias of its true period of 0.78 days by observations of e transiting in 2011.[23] This planet was the first instance of a fourth extrasolar planet in one system, and was the shortest-period planet until the discovery of PSR J1719-1438 b. The measurements that led to the discovery of this planet also confirmed the existence of 55 Cancri c.

In 2005, Jack Wisdom suggested that e actually had a period of 261 days and had a mass similar to that of Neptune in a 261-day orbit (corresponding to 0.77 AU in distance).[27] However, the planets were found to not conflict, and hence 55 Cancri f, the first occurrence of a fifth extrasolar planet in one system, was announced in 2007. With a similar mass to c, it has a 260-day orbit, towards the inner edge of 55 Cancri A's habitable zone.[28][29] The planet itself is not thought to be conducive to life, but hypothetical moons in principle could maintain at least microbial life.

The planet e's eccentricity is poorly defined; varying values between 0 and 0.4 does not significantly improve the fit, so an eccentricity of 0.2 was assumed. Taking interactions between the planets into account results in a near-zero orbital eccentricity.

Astrometric observations with the Hubble Space Telescope measured an inclination of 53° of the outer planet d,[26] though this result relies on the precise orbital parameters which have been substantially revised since this was published.[30] The observed transits of e suggest an orbit normal inclined within 9° to the line-of-light, and a possible detection of the transit of an extended atmosphere around 55 Cancri b would, if confirmed, imply that it too is in an orbit that is close to edge-on.[19] Between them, no measurement of c's nor f's inclination has been made. It had been thought that with five planets, the system cannot deviate far from coplanar in order to maintain stability.[29] An attempt to measure the spin-orbit misalignment of the innermost planet reported that it was in a nearly polar orbit,[31] but this interpretation of the data has since been challenged by a subsequent study, with noted inconsistencies between the implied and measured stellar rotation.[32]

The approximate ratios of periods of adjacent orbits are (proceeding outward): 1:20, 1:3, 1:6, 1:20. The nearly 1:3 ratio between 55 Cancri b and c is apparently a near resonance, rather than a genuine mean motion resonance.[29]

More planets are possible within the stable zone, between f and d at 0.9 to 3.8 AU with eccentricities below 0.4. Given hypothetical planet g of up to 50 Earth masses, stable mean motion resonance regions lie at 3f:2g, 2g:1d, and 3g:2d. As for the space outside d's orbit, its stability zone begins beyond 10 AU, though there is a stability zone between 8.6 - 9 AU due to a 2:1 resonance.[33]

The 55 Cancri A planetary system[23][34]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
e (Janssen) 8.63 ± 0.35 M⊕ 0.01560 ± 0.00011 0.736537 ± 0.000013 0.17 ± 0.04 83.4 ± 1.7° 2.00 ± 0.14 R⊕
b (Galileo) 0.825 ± 0.003 MJ 0.1148 ± 0.0008 14.6507 ± 0.0004 0.010 ± 0.003 ~85° —
c (Brahe) ≥0.171 ± 0.004 MJ 0.2403 ± 0.0017 44.364 ± 0.007 0.005 ± 0.003 — —
f (Harriot) ≥0.155 ± 0.008 MJ 0.781 ± 0.006 259.8 ± 0.5 0.30 ± 0.05 — —
d (Lipperhey) ≥3.82 ± 0.04 MJ 5.74 ± 0.04 5169 ± 53 0.014 ± 0.009 — —

Communication

A METI message was sent to 55 Cancri. It was transmitted from Eurasia's largest radar – 70-meter (230-foot) Eupatoria Planetary Radar. The message was named Cosmic Call 2; it was sent on July 6, 2003, and it will arrive at 55 Cancri in May 2044.[35]

See also

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.Vizier catalog entry
  2. ↑ van Belle, Gerard T.; von Braun, Kaspar (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". The Astrophysical Journal. 694 (2): 1085–1098. arXiv:0901.1206Freely accessible. Bibcode:2009ApJ...694.1085V. doi:10.1088/0004-637X/694/2/1085.
  3. ↑ Boyajian, Tabetha S.; et al. (July 2013), "Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations", The Astrophysical Journal, 771 (1): 31, arXiv:1306.2974Freely accessible, Bibcode:2013ApJ...771...40B, doi:10.1088/0004-637X/771/1/40, 40. See Table 3.
  4. ↑ Kovtyukh, V. V.; et al. (2003). "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios". Astronomy and Astrophysics. 411 (3): 559–564. arXiv:astro-ph/0308429Freely accessible. Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378.
  5. 1 2 3 4 5 6 Marcy, Geoffrey W.; et al. (2002). "A planet at 5 AU Around 55 Cancri". The Astrophysical Journal. 581 (2): 1375–1388. arXiv:astro-ph/0207294Freely accessible. Bibcode:2002ApJ...581.1375M. doi:10.1086/344298.
  6. 1 2 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal. 687 (2): 1264–1293. arXiv:0807.1686Freely accessible. Bibcode:2008ApJ...687.1264M. doi:10.1086/591785.
  7. 1 2 "IAU Catalog of Star Names". Retrieved 28 July 2016.
  8. 1 2 Raghavan, Deepak; et al. (2006). "Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems". The Astrophysical Journal. 646 (1): 523–542. arXiv:astro-ph/0603836Freely accessible. Bibcode:2006ApJ...646..523R. doi:10.1086/504823.
  9. 1 2 Butler, R. Paul; et al. (1997). "Three New 51 Pegasi Type Planets". The Astrophysical Journal Letters. 474 (2): L115–L118. Bibcode:1997ApJ...474L.115B. doi:10.1086/310444.
  10. ↑ Jean Schneider (2011). "Notes for Planet 55 Cnc b". Extrasolar Planets Encyclopaedia. Retrieved 8 October 2011.
  11. ↑ William I. Hartkopf & Brian D. Mason. "Addressing confusion in double star nomenclature: The Washington Multiplicity Catalog". United States Naval Observatory. Retrieved 2011-10-08.
  12. ↑ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
  13. ↑ NameExoWorlds The Process
  14. 1 2 Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
  15. 1 2 NameExoWorlds The Approved Names
  16. ↑ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  17. ↑ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  18. ↑ Eggenberger, A.; et al. (2003). "Planets in Binaries". Scientific Frontiers in Research on Extrasolar Planets. 294: 43–46. Bibcode:2003ASPC..294...43E.
  19. 1 2 3 D. Ehrenreich; et al. (October 2, 2012). "Hint of a transiting extended atmosphere on 55 Cancri b". Astronomy & Astrophysics. arXiv:1210.0531Freely accessible. Bibcode:2012A&A...547A..18E. doi:10.1051/0004-6361/201219981.
  20. ↑ von Braun, Kaspar; Tabetha, S. Boyajian; ten Brummelaar, Theo; Kane, Stephen R.; van Belle, Gerard T.; Ciardi, David R.; Raymond, Sean N.; López-Morales, Mercedes; McAlister, Harold A.; Schaefer, Gail (2011). "55 Cancri: Stellar Astrophysical Parameters, a Planet in the Habitable Zone, and Implications for the Radius of a Transiting Super-Earth". The Astrophysical Journal. 740 (1): 49–54. arXiv:1106.1152Freely accessible. Bibcode:2011ApJ...740...49V. doi:10.1088/0004-637X/740/1/49.
  21. ↑ Pasquini, Luca; Hatzes, Artie (2007-07-06). "Star Surface Polluted by Planetary Debris". ESO. Archived from the original on 30 September 2007. Retrieved 2007-11-08.
  22. ↑ Jayawardhana, Ray; et al. (2002). "New Submillimeter Limits on Dust in the 55 Cancri Planetary System". The Astrophysical Journal Letters. 570 (2): L93–L96. arXiv:astro-ph/0204140Freely accessible. Bibcode:2002ApJ...570L..93J. doi:10.1086/341101.
  23. 1 2 3 Winn, Joshua N.; et al. (2011). "A Super-Earth Transiting a Naked-Eye Star". The Astrophysical Journal Letters. 737 (1). article number L18. arXiv:1104.5230Freely accessible. Bibcode:2011ApJ...737L..18W. doi:10.1088/2041-8205/737/1/L18.
  24. ↑ Trilling, David E.; Brown, Robert H. (1998). "A circumstellar dust disk around a star with a known planetary companion" (PDF). Nature. 395 (6704): 775–777. Bibcode:1998Natur.395..775T. doi:10.1038/27389.
  25. ↑ Schneider, G.; et al. (2001). "NICMOS Coronagraphic Observations of 55 Cancri". The Astronomical Journal. 121 (1): 525–537. arXiv:astro-ph/0010175Freely accessible. Bibcode:2001AJ....121..525S. doi:10.1086/318050.
  26. 1 2 McArthur, Barbara E.; et al. (2004). "Detection of a NEPTUNE-mass planet in the ρ1 Cnc system using the Hobby-Eberly Telescope". The Astrophysical Journal Letters. 614 (1): L81–L84. arXiv:astro-ph/0408585Freely accessible. Bibcode:2004ApJ...614L..81M. doi:10.1086/425561.
  27. ↑ Wisdom, J. (2005). "Evidence of a Neptune-Sized Planet in the ρ1 Cancri System". Bulletin of the American Astronomical Society. 37: 525. Bibcode:2005DDA....36.0508W.
  28. ↑ "Astronomers Discover Record Fifth Planet Around Nearby Star 55 Cancri". Sciencedaily.com. November 6, 2007. Archived from the original on 26 September 2008. Retrieved 2008-09-14.
  29. 1 2 3 Fischer, Debra A.; et al. (2008). "Five Planets Orbiting 55 Cancri". The Astrophysical Journal. 675 (1): 790–801. arXiv:0712.3917Freely accessible. Bibcode:2008ApJ...675..790F. doi:10.1086/525512.
  30. ↑ Nelson, Benjamin E.; Ford, Eric B.; Wright, Jason T.; Fischer, Debra A.; von Braun, Kaspar; Howard, Andrew W.; Payne, Matthew J.; Dindar, Saleh (2014). "The 55 Cancri planetary system: fully self-consistent N-body constraints and a dynamical analysis". Monthly Notices of the Royal Astronomical Society. 441 (1): 442–451. arXiv:1402.6343Freely accessible. Bibcode:2014MNRAS.441..442N. doi:10.1093/mnras/stu450.
  31. ↑ Vincent Bourrier; Guillaume Hébrard (2014). "Detecting the spin-orbit misalignment of the super-Earth 55 Cnc e". arXiv:1406.6813Freely accessible [astro-ph.EP].
  32. ↑ Mercedes Lopez-Morales; Amaury H. M. J. Triaud; Florian Rodler; Xavier Dumusque; Lars A. Buchhave; A. Harutyunyan; Sergio Hoyer; Roi Alonso; Michael Gillon; Nathan A. Kaib; David W. Latham; Christophe Lovis; Francesco Pepe; Didier Queloz; Sean N.Raymond; Damien Segransan; Ingo P. Waldmann; Stephane Udry (2014). "Rossiter-McLaughlin Observations of 55 Cnc e". arXiv:1408.2007Freely accessible [astro-ph.EP].
  33. ↑ Raymond, Sean N.; et al. (2008). "A dynamical perspective on additional planets in 55 Cancri". The Astrophysical Journal. 689: 478–491. arXiv:0808.3295Freely accessible. Bibcode:2008ApJ...689..478R. doi:10.1086/592772.
  34. ↑ Dawson, Rebekah I.; Fabrycky, Daniel C. "Radial velocity planets de-aliased. A new, short period for Super-Earth 55 Cnc e". The Astrophysical Journal. 722: 937–953. arXiv:1005.4050Freely accessible. Bibcode:2010ApJ...722..937D. doi:10.1088/0004-637X/722/1/937.
  35. ↑ "Передача и поиски разумных сигналов во Вселенной". Cplire.ru. Retrieved 2008-09-14.

Further reading

External links

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Coordinates: 08h 52m 35.8s, 28° 19′ 51″

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