In 2007, Patrick Wilset al. discovered that NSVS 14256825 is an eclipsing binary, by examining the Northern Sky Variability Survey (NSVS) data. They also classified it as anHW Virginis type star, a binary pair in which variability arises from one star reflecting the light of the other as they orbit each other.[6][7][8]
NSVS 14256825 has been extremely well-studied usingphotometry,[9] but the resulting models often contradict each other, even with similar statistical significance,[10] or with data that are collected later.[9] Many studies have found that this system exhibitseclipse timing variations (ETVs) that are significant, cyclic[9] and not explainable by other stellar mechanisms such as theApplegate mechanism.[11] In 2012, it was found that the orbit of NSVS 14256825 was increasing at a rate of12×10−12 days per orbit.[12]
Initially, in 2012 it was claimed that two giant planets were in orbit around the binary, with masses of 2.9 and 8.1 times the mass ofJupiter orbiting with periods of 3.5 and 6.9 years respectively.[1] Another paper claimed the existence of one planet with a mass 12 times that of Jupiter, in a 20-year orbit.[13] However, subsequent studies have come up with different results with masses up to15MJ[11] and periods down to 8.83 years.[14] Studies also do not agree on whether one substellar body can explain the ETVs, or whether additional companions are necessary, but further research is needed to obtain better coverage of data.[15]
^Kupfer, T.; Geier, S.; Heber, U.; Østensen, R. H.; Barlow, B. N.; Maxted, P. F. L.; Heuser, C.; Schaffenroth, V.; Gänsicke, B. T. (2015). "Hot subdwarf binaries from the MUCHFUSS project. Analysis of 12 new systems and a study of the short-period binary population".Astronomy and Astrophysics.576: A44.arXiv:1501.03692.Bibcode:2015A&A...576A..44K.doi:10.1051/0004-6361/201425213.S2CID53724563.
^Wils, Patrick; di Scala, Giorgio; Otero, Sebastian A. (October 2007)."NSVS 14256825: A New HW Vir Type System"(PDF).Information Bulletin on Variable Stars.5800:1–5. Retrieved22 November 2024.
^"V1828 Aql".The International Variable Star Index. AAVSO. Retrieved22 November 2024.
^abWoźniak, P. R.; Vestrand, W. T.; Akerlof, C. W.; Balsano, R.; Bloch, J.; Casperson, D.; Fletcher, S.; Gisler, G.; Kehoe, R.; Kinemuchi, K.; Lee, B. C.; Marshall, S.; McGowan, K. E.; McKay, T. A.; Rykoff, E. S.; Smith, D. A.; Szymanski, J.; Wren, J. (2004). "Northern Sky Variability Survey: Public Data Release".The Astronomical Journal.127 (4):2436–2449.arXiv:astro-ph/0401217.Bibcode:2004AJ....127.2436W.doi:10.1086/382719.S2CID2974543.
^abcPulley, D.; Faillace, G.; Smith, D.; Watkins, A.; von Harrach, S. (2018). "The quest for stable circumbinary companions to post-common envelope SDB eclipsing binaries. Does the observational evidence support their existence?".Astronomy and Astrophysics.611: 611.arXiv:1711.03749.Bibcode:2018A&A...611A..48P.doi:10.1051/0004-6361/201731125.S2CID54997940.
^Beuermann, K.; Breitenstein, P.; Debski, B.; Diese, J.; Dubovsky, P. A.; Dreizler, S.; Hessman, F. V.; Hornoch, K.; Husser, T. -O.; Pojmanski, G.; Wolf, M.; Woźniak, P. R.; Zasche, P.; Denk, B.; Langer, M.; Wagner, C.; Wahrenberg, D.; Bollmann, T.; Habermann, F. N.; Haustovich, N.; Lauser, M.; Liebing, F.; Niederstadt, F. (2012). "The quest for companions to post-common envelope binaries. II. NSVS14256825 and HS0705+6700".Astronomy and Astrophysics.540: A8.arXiv:1202.5990.Bibcode:2012A&A...540A...8B.doi:10.1051/0004-6361/201118105.S2CID119267859.
