V1400 Centauri

Coordinates: Sky map 14h 07m 47.930s, −39° 45′ 42.77″
Source: Wikipedia, the free encyclopedia.
(Redirected from 1SWASP J140747.93-394542.6)

V1400 Centauri

V1400 Centauri imaged by the Dark Energy Survey
Observation data
Epoch J2000      Equinox J2000
Constellation Centaurus
Right ascension 14h 07m 47.92976s[1]
Declination −39° 45′ 42.7671″[1]
Apparent magnitude (V) 12.2–15.6[2]
Characteristics
Evolutionary stage Pre-main sequence[3]
Spectral type K5 IVe Li[3][4]
Variable type rotational T Tau and eclipsing[2]
Astrometry
Radial velocity (Rv)5.904±0.151[4] km/s
Proper motion (μ) RA: −23.108±0.015 mas/yr[1]
Dec.: −21.048±0.017 mas/yr[1]
Parallax (π)7.2351 ± 0.0140 mas[1]
Distance450.8 ± 0.9 ly
(138.2 ± 0.3 pc)
Details
MassGaia DR3 with magnetism:[5]
0.977+0.023
−0.045 M☉
Gaia DR3 without magnetism:[5]
0.891+0.062
−0.144 M☉
Gaia DR2:[6]: 2 
0.95±0.10 M☉
Radius1.0661+0.0062
−0.0139[7] R☉
Luminosity0.3431+0.0067
−0.0064[7] L☉
Surface gravity (log g)4.302+0.0243
−0.0243[7] cgs
Temperature4343+24
−29[7] K
Metallicity [Fe/H]−0.1903+0.0448
−0.0422[7] dex
Rotation3.206±0.002 d[8]: 6 [a]
Rotational velocity (v sin i)14.6±0.4[9] km/s
Age~16[3] or 21.38+4.30
−7.60[6]: 2  Myr
Other designations
V1400 Cen, GSC 07807-00004, 2MASS J14074792–3945427, WISE J140747.91–394542.9, 1SWASP J140747.93–394542.6, ASAS J140748–3945.7[4]
Database references
SIMBADdata

V1400 Centauri, also known as 1SWASP J140747.93−394542.6 or simply J1407, is a young, pre-main-sequence star that was eclipsed by the likely free-floating substellar object J1407b in April–June 2007. With an age around 20 million years, the star is about as massive as the Sun and is located in the constellation Centaurus at a distance of 451 light-years away from the Sun. V1400 Centauri is a member of Upper Centaurus–Lupus subgroup of the Scorpius–Centaurus association, a group of young, comoving stars close to the Sun.

Name and catalogue history

The star has been catalogued in as early as the 1990s by the Hubble Guide Star Catalog, which identified the star and measured its position in a pair of photographic plates taken in 1974 and 1979.[10] The star has been catalogued by other sky surveys, including the All Sky Automated Survey (ASAS), Two Micron All-Sky Survey (2MASS), Super Wide Angle Search for Planets (1SWASP), and the Wide-field Infrared Survey Explorer (WISE).[4] Typically in these catalogues, the star is given designations such as 1SWASP J140747.93–394542.6, which comprises the survey name followed by the star's location in equatorial coordinates.[4] As such designations can be unwieldy, researchers simply call the star "J1407".[3]: 5 [11] The star was given the official variable star designation V1400 Centauri in 2015, when it was added to the International Astronomical Union's General Catalogue of Variable Stars.[12] A 2018 research paper on stars with unusual dimming periods nicknamed V1400 Centauri "Mamajek's Object", after the astronomer Eric Mamajek who identified the star's unusual dimming in 2007.[13]

Stellar properties

Location and age

V1400 Centauri is located in the constellation Centaurus.
V1400 Centauri is located in the constellation Centaurus.
V1400 Centauri
class=notpageimage|
Location of V1400 Centauri in the constellation Centaurus

V1400 Centauri is located in the constellation Centaurus, about 40 degrees south of the celestial equator.[4] The most recent parallax measurements by the Gaia spacecraft indicate V1400 Centauri is located 450.8 ± 0.9 light-years (138.2 ± 0.3 parsecs) from the Sun.[1] Observations of V1400 Centauri's position over time have shown that it has a southwestward[b] proper motion consistent with that of the Scorpius–Centaurus association, an OB association of young stars with ages between 11–17 million years and distances between 380–470 ly (118–145 pc) from the Sun.[3]: 4  The Scorpius–Centaurus association is the nearest OB association to the Sun, and is believed to have formed out of a molecular cloud that has since been blown away by the stellar winds of the association's most massive stars.[14]: 236, 250 

V1400 Centauri is closest to the Upper Centaurus–Lupus subgroup of the Scorpius–Centaurus association, which has an age range of 14–18 million years and distance range of 380–460 ly (115–141 pc).[3]: 5-6  Given V1400 Centauri's similar distance and proper motion, it very likely belongs to the Scorpius–Centaurus association, which would mean it must be a young star within the age range of the Upper Centaurus–Lupus subgroup.[3]: 5-6  A 2012 estimate of V1400 Centauri's age assumes it is equal to 16 million years,[3]: 6  the mean age of the Upper Centaurus–Lupus subgroup, while a 2018 estimate from Gaia measurements puts the star's age at 21.38+4.30
−7.60 million years.[6]: 2 

Spectral type and physical characteristics

V1400 Centauri is a pre-main sequence star of spectral class K5 IVe Li.[4][3]: 5  "K" means V1400 Centauri is an orange K-type star, and the adjoining number "5" ranks V1400 Centauri's relative temperature on a scale of 9 (coolest) to 0 (hottest) for K-type stars. V1400 Centauri is given the subgiant luminosity class "IV", because it has a brighter luminosity than K-type main-sequence stars (luminosity class V).[3]: 5 [c] The letter "e" indicates V1400 Centauri exhibits weak hydrogen-alpha emission lines in its visible light spectrum.[3]: 5  Lastly, "Li" indicates V1400 Centauri is abundant in lithium.[3]: 5 

Measurements from the Gaia spacecraft's third and most recent data release (Gaia DR3) indicate V1400 Centauri is about 7% larger than the Sun in radius (1.07 R☉; 740,000 km; 460,000 mi),[7] but is slightly less massive than the Sun.[5][6]: 2  Depending on whether magnetic effects are taken into account in V1400 Centauri's stellar evolution or not, the star's mass could be either 0.98 M☉ or 0.89 M☉, respectively.[5]: 4  Young stars tend to be magnetically active,[15] and neglecting their magnetic effects results in an underestimation of their mass.[5]: 4, 9  An older estimate of V1400 Centauri's mass from Gaia's second data release (Gaia DR2) in 2018 gives 0.95 M☉, but does not take magnetic effects into account.[6]: 2 

V1400 Centauri is cooler and less luminous than the Sun, with an effective temperature of about 4,300 K (4,030 °C; 7,280 °F) and a luminosity about 34% that of the Sun.[7] V1400 Centauri has an estimated surface gravity of about 200 m/s2 (over 20 times the gravity of Earth), based on Gaia measurements of the star's brightness, distance, and color.[1][d] Gaia measurements also indicate V1400 Centauri has a lower metallicity than the Sun.[1][e] Viewed from Earth, V1400 Centauri appears marginally redder than a typical K5-type star due to light extinction by interstellar dust between Earth and the star.[f] The star does not exhibit excess thermal emission in near- and mid-infrared wavelengths and lacks strong emission lines in its spectrum, which indicates it lacks a substantial accretion disk or protoplanetary disk.[3]: 10 

Rotation and variability

Like most young stars, V1400 Centauri rotates rapidly with a rotation period of approximately 3.2 days.[3]: 8  The rapid rotation of V1400 Centauri strengthens its magnetic field via the dynamo process, which leads to the formation of starspots on its surface.[8]: 6  As V1400 Centauri rotates, its starspots come into and out of view, causing the star's brightness to periodically fluctuate by 5%, or about 0.1 magnitudes in amplitude.[8]: 2  The star's rotation period varies by 0.02 days over a 5.4-year-long magnetic activity cycle, due to the long-term movement of starspots across the star's differentially rotating surface.[8]: 6 [16]: 2847  V1400 Centauri is known to emit soft X-rays[3]: 8  due to its corona being heated by its rotationally-strengthened magnetic field.[17] Because of its young age, starspot variability, and lack of dust accretion, V1400 Centauri is classified as a weak-lined T Tauri variable.[9]: 412 [2]

Spectroscopic measurements of Doppler broadening in V1400 Centauri's spectral absorption lines indicate the star has a projected rotational velocity of 14.6±0.4 km/s.[9]: 415–416  Given V1400 Centauri's rotation period, radius, and temperature, the star's true equatorial rotation velocity is 15.7±1.7 km/s,[9]: 418  which indicates that the star's rotation axis is inclined 68°±10° with respect to Earth's line of sight.[9]: 419 

2007 eclipse by J1407b

Main article: J1407b
Visual-band light curve of V1400 Centauri, showing the 2007 eclipse. The main plot shows the SuperWASP data.[18] The inset plot, adapted from Mamajek et al.,[3] shows the data near mid-eclipse. The purple markers show the pairs of small brightness dips due to eclipses by rings.
Simulation of J1407b eclipsing V1400 Centauri during 2007. The light curve plot below illustrates V1400 Centauri's brightness changes during the eclipse. The ring structure of J1407b and the orange light curve represents a best-fit model to SuperWASP's photometric data, which are shown in yellow points.

During 7 April to 4 June 2007,[g] telescopes of the Super Wide Angle Search for Planets (SuperWASP) and All Sky Automated Survey (ASAS) projects recorded V1400 Centauri undergoing a series of significant dimming events for 56 days.[8] The pattern of these dimming events was complex yet nearly symmetrical, indicating they were caused by an opaque, disk-like structure eclipsing the star.[3]: 5  The object that eclipsed V1400 Centauri is now known as J1407b, a substellar object surrounded by a dusty circumplanetary disk about 90 million kilometers (56 million miles) in radius.

V1400 Centauri's eclipse by J1407b was discovered on 3 December 2010 by Mark Pecaut,[3]: 5  who at the time was a graduate student under the supervision of Eric E. Mamajek at the University of Rochester.[20] Mamajek, Pecaut, and collaborators announced the discovery in 2012.[20] Mamajek's team initially hypothesized that J1407b is a ringed exoplanet or brown dwarf orbiting the star,[3]: 8  but that has since been disfavored by later studies. V1400 Centauri does not show repeating eclipses, telescope observations showed no orbiting companions, and the disk of J1407b would be unstable if it orbited the star, which suggests that J1407b likely does not orbit V1400 Centauri and is instead a free-floating object that coincidentally passed in front of the star.[11]: 2  In this case, J1407b's coincidental eclipse of V1400 Centauri would be considered an extremely rare event that will never happen again.[21]: 9 [20]

High-resolution imaging by the Atacama Large Millimeter Array (ALMA) in 2017 revealed a single object near V1400 Centauri, which might be J1407b. The object's distance from V1400 Centauri appears to match the expected distance travelled by J1407b if it was a free-floating object. The object's brightness is suggestive of a dusty circumplanetary disk surrounding a planetary-mass object below 6 Jupiter masses. However, the object has only been observed by ALMA once, so it is not yet known whether it is a moving foreground object or a stationary background galaxy.[11] Recent observations by ALMA in June and July 2024 will confirm whether this object is J1407b or not.[22]

See also

Notes

  1. ^ 3.206±0.002 d is the median rotation period of V1400 Centauri throughout its 5.4-year magnetic activity cycle.[8]: 6 
  2. ^ Proper motion is split into right ascension (RA) and declination (Dec) components. By convention, positive RA is eastward and positive Dec is northward in the equatorial coordinate system. The measured proper motion components of V1400 Centauri are −23.108±0.015 mas/yr and −21.048±0.017 mas/yr in RA and Dec, respectively.[1] Since both RA and Dec components of V1400 Centauri's proper motion are negative, its proper motion is pointed towards the west and south directions, hence southwest.
  3. ^ The term "subgiant" and its associated luminosity class "IV" can either refer to the life stage between the main-sequence and giant phases near the end of a star's life, or it can strictly refer to a star's luminosity only. In the case of V1400 Centauri, the latter definition is used since it is appropriate for the star's young age.
  4. ^ The Gaia DR3 table gives log g = 4.302 as the base 10 logarithm of surface gravity in cgs units.[1] Raising 10 to the power of log g gives the star's surface gravity g in cgs units of cm/s2. Converting the result to the SI acceleration units of m/s2 gives g ≈ 200.4 m/s2 for V1400 Centauri's surface gravity.
  5. ^ The Gaia DR3 table gives the [Fe/H] metallicity (iron abundance relative to the Sun) as a base 10 logarithmic quantity. V1400 Centauri has a negative [Fe/H] metallicity of –0.1903, which indicates a lower iron abundance than the Sun.[1]
  6. ^ The latest estimate for V1400 Centauri's extinction reddening index is E(GBP–GRP) = 0.0414+0.0518
    −0.0314     mag, from Gaia DR3 (2022).[7] Mamajek et al. (2012) claimed V1400 Centauri is consistent with being slightly reddened,[3]: 5  whereas van Werkhoven et al. (2014) claimed it is statistically consistent with being unreddened.[16]: 2848 
  7. ^ According to van Werkhoven et al. (2014), J1407b's eclipse start and end times are Modified Julian Date (MJD) 54197 and 54255, respectively.[16]: 2847  To convert these to Julian date (JD), add 2400000.5 to MJD. This gives JD 2454197.5 and JD 2454255.5 for the eclipse start and end times, respectively. Converting these JD dates to calendar dates gives 7 April 2007 UTC and 4 June 2007 UTC, respectively.[19]

References

  1. ^ a b c d e f g h i j Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c "V1400 Cen". International Variable Star Index. AAVSO. Archived from the original on 1 August 2023. Retrieved 1 August 2023.
  3. ^ a b c d e f g h i j k l m n o p q r s t Mamajek, Eric E.; Quillen, Alice C.; Pecaut, Mark J.; Moolekamp, Fred; Scott, Erin L.; Kenworthy, Matthew A.; et al. (March 2012). "Planetary Construction Zones in Occultation: Discovery of an Extrasolar Ring System Transiting a Young Sun-like Star and Future Prospects for Detecting Eclipses by Circumsecondary and Circumplanetary Disks". The Astronomical Journal. 143 (3): 15. arXiv:1108.4070. Bibcode:2012AJ....143...72M. doi:10.1088/0004-6256/143/3/72. S2CID 55818711. 72.
  4. ^ a b c d e f g "V* V1400 Cen". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 23 May 2024.
  5. ^ a b c d e Fernandes, Rachel B.; Hardegree-Ullman, Kevin K.; Pascucci, Ilaria; Bergsten, Galen J.; Mulders, Gijs D.; Cunha, Katia; et al. (October 2023). "Using Photometrically Derived Properties of Young Stars to Refine TESS's Transiting Young Planet Survey Completeness". The Astronomical Journal. 166 (4): 12. arXiv:2308.13039. Bibcode:2023AJ....166..175F. doi:10.3847/1538-3881/acf4f0. 175. Gaia DR3 data table and mass estimates for V1400 Centauri at VizieR.
  6. ^ a b c d e Mentel, R. T.; Kenworthy, M. A.; Cameron, D. A.; Scott, E. L.; Mellon, S. N.; Hudec, R.; et al. (November 2018). "Constraining the period of the ringed secondary companion to the young star J1407 with photographic plates". Astronomy & Astrophysics. 619: 7. arXiv:1810.05171. Bibcode:2018A&A...619A.157M. doi:10.1051/0004-6361/201834004. S2CID 55015149. A157.
  7. ^ a b c d e f g h Gaia Collaboration (May 2022). "VizieR Online Data Catalog: Gaia DR3 Part 1. Main source". VizieR. I/355. Centre de données astronomiques de Strasbourg. Bibcode:2022yCat.1355....0G. doi:10.26093/cds/vizier.1355.
  8. ^ a b c d e f Barmentloo, S.; Dik, C.; Kenworthy, M. A.; Mamajek, E. E.; Hambsch, F.-J.; Reichart, D. E.; et al. (August 2021). "A search for transiting companions in the J1407 (V1400 Cen) system". Astronomy & Astrophysics. 652: 8. arXiv:2106.15902. Bibcode:2021A&A...652A.117B. doi:10.1051/0004-6361/202140768. S2CID 235683556. A117.
  9. ^ a b c d e Kenworthy, M. A.; Lacour, S.; Kraus, A.; Triaud, A. H. M. J.; Mamajek, E. E.; Scott, E. L.; et al. (January 2015). "Mass and period limits on the ringed companion transiting the young star J1407". Monthly Notices of the Royal Astronomical Society. 446 (1): 411–427. arXiv:1410.6577. Bibcode:2015MNRAS.446..411K. doi:10.1093/mnras/stu2067.
  10. ^ Lasker, B. M.; Russell, J. L.; Jenker, H.; Sturch, C. R.; McLean, B. J.; Shara, M. M. (February 1996). "VizieR Online Data Catalog: The HST Guide Star Catalog, Version 1.1". VizieR. I/220. Centre de données astronomiques de Strasbourg. Bibcode:1996yCat.1220....0L.
  11. ^ a b c Kenworthy, M. A.; Klaasen, P. D.; Min, M.; van der Marel, N.; Bohn, A. J.; Kama, M.; et al. (January 2020). "ALMA and NACO observations towards the young exoring transit system J1407 (V1400 Cen)". Astronomy & Astrophysics. 633: 6. arXiv:1912.03314. Bibcode:2020A&A...633A.115K. doi:10.1051/0004-6361/201936141. A115.
  12. ^ Kazarovets, E. V; Samus, N. N; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (October 2015). "The 81st Name-List of Variable Stars. Part I - RA 00h to 17h30" (PDF). Information Bulletin on Variable Stars. 6151 (1): 22. Bibcode:2015IBVS.6151....1K.
  13. ^ Saito, R. K.; Minniti, D.; Ivanov, V. D.; Catelan, M.; Gran, F.; Baptista, R.; et al. (February 2019). "VVV-WIT-07: another Boyajian's star or a Mamajek's object?". Monthly Notices of the Royal Astronomical Society. 482 (4): 5000–5006. arXiv:1811.02265. Bibcode:2019MNRAS.482.5000S. doi:10.1093/mnras/sty3004.
  14. ^ Preibisch, Thomas; Mamajek, Eric (December 2008). "The Nearest OB Association: Scorpius-Centaurus (Sco OB2)" (PDF). In Reipurth, Bo (ed.). Handbook of Star Forming Regions, Volume II: The Southern Sky. Vol. 5. ASP Monograph Publications. pp. 235–284. arXiv:0809.0407. Bibcode:2008hsf2.book..235P. ISBN 978-1-58381-671-4. Retrieved 14 July 2024.
  15. ^ Mathur, Savita; Claytor, Zachary R.; Santos, Ângela R. G.; García, Rafael A.; Amard, Louis; Bugnet, Lisa; et al. (June 2023). Evolution of rotation and magnetic activity of solar-like stars with age:magneto-(gyro-)chronology. PLATO Stellar Science Conference 2023. Milazzo, Italy. Bibcode:2023plat.confE..36M. doi:10.5281/zenodo.8140785. 404.04.
  16. ^ a b c van Werkhoven, T. I. M.; Kenworthy, M. A.; Mamajek, E. E. (July 2014). "Analysis of 1SWASP J140747.93-394542.6 eclipse fine-structure: hints of exomoons". Monthly Notices of the Royal Astronomical Society. 441 (4): 2845–2854. Bibcode:2014MNRAS.441.2845V. doi:10.1093/mnras/stu725.
  17. ^ "Young Stars and Star Clusters". Chandra X-ray Observatory. NASA. 10 August 2012. Retrieved 14 July 2024.
  18. ^ "Search SuperWASP Time Series". NASA Exoplanet Archive. NASA. Archived from the original on 27 November 2022. Retrieved 27 November 2022. (In the "Include location search around coordinates / object names" box, type "V1400 Centauri" and then click "Submit Search".)
  19. ^ "JD Date/Time Converter". Solar System Dynamics. JPL/NASA. Retrieved 25 July 2024.
  20. ^ a b c Kenworthy, Matthew A. (27 July 2024). "J1407b". Archived from the original on 28 July 2024. Retrieved 28 July 2024.
  21. ^ Kenworthy, M. A.; Mamajek, E. E. (February 2015). "Modeling giant extrasolar ring systems in eclipse and the case of J1407b: sculpting by exomoons?". The Astrophysical Journal. 800 (2): 10. arXiv:1501.05652. Bibcode:2015ApJ...800..126K. doi:10.1093/mnras/stu2067. S2CID 56118870. 126.
  22. ^ "ALMA Science Archive". National Radio Astronomy Observatory. Archived from the original on 24 July 2024. Retrieved 23 July 2024.
Wikimedia Commons has media related to V1400 Centauri.
Retrieved from "https://en.wikipedia.org/w/index.php?title=V1400_Centauri&oldid=1239563673"