{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,1,8]],"date-time":"2026-01-08T05:05:45Z","timestamp":1767848745205,"version":"3.49.0"},"reference-count":30,"publisher":"World Scientific Pub Co Pte Lt","issue":"12","content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Int. J. Mod. Phys. D"],"published-print":{"date-parts":[[2006,12]]},"abstract":"<jats:p>The evidence for supermassive Kerr black holes in galactic centers is strong and growing, but only the detection of gravitational waves will convincingly rule out other possibilities to explain the observations. The Kerr space\u2013time is completely specified by the first two multipole moments: mass and angular momentum. This is usually referred to as the \"no-hair theorem,\" but it is really a \"two-hair\" theorem. If general relativity is the correct theory of gravity, the most plausible alternative to a supermassive Kerr black hole is a rotating boson star. Numerical calculations indicate that the space\u2013time of rotating boson stars is determined by the first three multipole moments (\"three-hair theorem\"). The Laser Interferometer Space Antenna (LISA) could accurately measure the oscillation frequencies of these supermassive objects. We propose to use these measurements to \"count their hair,\" unambiguously determining their nature and properties.<\/jats:p>","DOI":"10.1142\/s0218271806009637","type":"journal-article","created":{"date-parts":[[2007,3,12]],"date-time":"2007-03-12T09:56:23Z","timestamp":1173693383000},"page":"2209-2216","source":"Crossref","is-referenced-by-count":54,"title":["SUPERMASSIVE BLACK HOLES OR BOSON STARS? HAIR COUNTING WITH GRAVITATIONAL WAVE DETECTORS"],"prefix":"10.1142","volume":"15","author":[{"given":"EMANUELE","family":"BERTI","sequence":"first","affiliation":[{"name":"McDonnell Center for the Space Sciences, Department of Physics, Washington University, St. Louis, MO 63130, USA"}]},{"given":"VITOR","family":"CARDOSO","sequence":"additional","affiliation":[{"name":"Department of Physics and Astronomy, The University of Mississippi, MS 38677-1848, USA"}]}],"member":"219","published-online":{"date-parts":[[2012,1,25]]},"reference":[{"key":"rf1","doi-asserted-by":"publisher","DOI":"10.1088\/1367-2630\/7\/1\/199"},{"key":"rf2","doi-asserted-by":"publisher","DOI":"10.1038\/nature01121"},{"key":"rf3","doi-asserted-by":"publisher","DOI":"10.1086\/380188"},{"key":"rf4","doi-asserted-by":"publisher","DOI":"10.1086\/374804"},{"key":"rf5","doi-asserted-by":"publisher","DOI":"10.1086\/427175"},{"key":"rf6","doi-asserted-by":"publisher","DOI":"10.1038\/nature04205"},{"key":"rf7","doi-asserted-by":"publisher","DOI":"10.1086\/311194"},{"key":"rf8","doi-asserted-by":"publisher","DOI":"10.1111\/j.1745-3933.2006.00135.x"},{"key":"rf9","doi-asserted-by":"publisher","DOI":"10.1038\/nature01121"},{"key":"rf10","doi-asserted-by":"publisher","DOI":"10.1086\/500930"},{"key":"rf11","doi-asserted-by":"publisher","DOI":"10.1051\/0004-6361:20021645"},{"key":"rf12","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRevD.52.5707"},{"key":"rf13","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRevD.56.1845"},{"key":"rf14","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRevD.71.044015"},{"key":"rf15","doi-asserted-by":"publisher","DOI":"10.1088\/0264-9381\/23\/12\/013"},{"key":"rf16","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRevD.73.064030"},{"key":"rf17","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRevD.62.104012"},{"key":"rf18","doi-asserted-by":"publisher","DOI":"10.1088\/0264-9381\/20\/20\/201"},{"key":"rf19","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRevD.57.4535"},{"key":"rf20","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRev.172.1331"},{"key":"rf21","doi-asserted-by":"publisher","DOI":"10.1103\/PhysRev.187.1767"},{"key":"rf22","doi-asserted-by":"crossref","first-page":"601","DOI":"10.1142\/S0218271800000608","volume":"9","author":"Schunck F. 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