Michael Farfán Stopani is a retired American soccer player. Played club soccer with the La Jolla Nomads of San Diego where he captured numerous team titles, including the 2002 national championship, he played in the Youth World Championships in Japan in 2000. Farfan played for Castle Park High School in Chula Vista, California where he won All-CIF honors as an underclassman, he played for Edison Academic Center in Bradenton, Florida while training for the United States U-17 team. As a member of the U-17 team, Farfan played in the 2005 Youth World Cup. After a two-year residency on the United States U-17 team, he enrolled at Fullerton State in the Spring of 2006. Farfan enrolled in the University of North Carolina in January 2009, he scored five goals with the Tar Heels, with three coming in the first four games, had four assists. While at North Carolina, he was named All-ACC First Team. During his college years Farfan played extensively in the USL Premier Development League, for Orange County Blue Star, Ventura County Fusion, the Los Angeles Legends, the Ogden Outlaws.
On January 13, 2011, Farfan was drafted in the second round in the 2011 MLS SuperDraft by the Philadelphia Union. He made his professional debut on April 6, 2011 in a Lamar Hunt U. S. Open Cup game against D. C. United and scored his first professional goal – a 25-yard drive from outside the box – on May 21, 2011 in a 2–1 win over Chicago Fire, he was part of the MLS Team of Week 10 for this performance. After three seasons in Philadelphia, Farfan was sold to Cruz Azul of Liga MX ahead of the 2014 Clasura, he scored in his debut with Cruz Azul against Pachuca. Farfan was released by Cruz Azul just 6-months into his 3-year deal. Farfan was signed by D. C. United on February 10, 2015. Farfan signed with Seattle Sounders FC on January 20, 2016. On February 24, 2017, Farfan announced his retirement via Facebook. Updated March 13, 2015 Michael's brother, Gabriel Farfán, is a professional soccer player for Miami FC. Cruz AzulCONCACAF Champions League: 2013–14 Major League Soccer All-Star Team: 2012 Michael Farfan at Major League Soccer UNC bio Michael Farfan – FIFA competition record
BV Centauri is a cataclysmic variable binary star in the constellation Centaurus. It is a dwarf nova, undergoes rapid increases in brightness that are recurrent with a mean period of 150 days; this period seems to have increased in the last few decades. During quiescence, its visual apparent magnitude is about 13, with variations of a few tenths of magnitude over an orbit due to differences in the star's visible surface area, brightening to a maximum magnitude of 10.7 during outbursts. From its luminosity, it is estimated. A Gaia parallax of 2.81 mas has been measured. Cataclysmic variables are short-period binary systems in which a white dwarf primary accretes matter from a secondary star. For BV Centauri, the white dwarf and its companion have estimated masses of 1.18 and 1.05 times the mass of the Sun respectively. The secondary is a conventional star with a spectral type of G5-G8IV-V and it is assumed to contribute to half of the visual luminosity of the system, it is thought to have a radius of 1.4 R☉ and so to be evolved away from the zero age main sequence.
The reconstruction of its surface by Doppler imaging revealed it to be a magnetically active star, with about 25% of its surface covered in starspots which are much more abundant on the hemisphere facing the white dwarf. Furthermore, a prominence was detected above the secondary star's surface in the side facing the white dwarf; the white dwarf primary can be observed at ultraviolet wavelengths where it is the strongest source. Any accretion disk in the system appears faint; the system has a period of 0.611179 days, one of the longest periods for a dwarf nova, is inclined by 53 ± 4° in relation to the plane of the sky. It has been noted that BV Centauri's light curve during outbursts has anomalous behavior for a dwarf nova, with a long interval of up to 15 days before reaching peak brightness and no plateau at maximum brightness, it has been compared to the classic nova GK Persei. Based on this, it has been proposed that BV Centauri could have generated an unobserved nova outburst in the 19th century, missed by the observers at the time