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005    20190405013643.8 
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007    cr cnu---unuuu 
008    070807s2006    enka    ob    001 0 eng d 
019    159957466|a171124404|a181092549|a506243504|a647519134
       |a813436777|a847969796|a1033739599 
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020    0511536208|q(electronic book) 
020    9786610550531 
020    6610550530 
020    |z0521855578 
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020    |z9780511224423 
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024 3  |z9780521855570 
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037    |bOverDrive, Inc.|nhttp://www.overdrive.com 
037    0634DCBF-FB59-4EC4-81F4-52890D66B861|bOverDrive, Inc.
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040    N$T|beng|epn|cN$T|dYDXCP|dOCLCQ|dOCLCO|dTEFOD|dUAB|dIDEBK
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049    RIDW 
050  4 QB821|b.E34 2006eb 
072  7 SCI|x004000|2bisacsh 
082 04 523.841|222 
084    US 5000|2rvk 
090    QB821|b.E34 2006eb 
100 1  Eggleton, P. P.|q(Peter P.),|d1940-|0https://id.loc.gov/
       authorities/names/n84200909 
245 10 Evolutionary processes in binary and multiple stars /
       |cPeter Eggleton. 
264  1 Cambridge, UK ;|aNew York :|bCambridge University Press,
       |c2006. 
300    1 online resource (viii, 322 pages) :|billustrations. 
336    text|btxt|2rdacontent 
337    computer|bc|2rdamedia 
338    online resource|bcr|2rdacarrier 
340    |gpolychrome|2rdacc 
347    text file|2rdaft 
490 1  Cambridge astrophysics series ;|v40 
504    Includes bibliographical references (pages 304-314) and 
       indexes. 
520    Binary systems of stars are as common as single stars. 
       Stars evolve primarily by nuclear reactions in their 
       interiors, but a star with a binary companion can also 
       have its evolution influenced by the companion. Multiple 
       star systems can exist stably for millions of years, but 
       can ultimately become unstable as one star grows in radius
       until it engulfs another. This volume, first published in 
       2006, discusses the statistics of binary stars; the 
       evolution of single stars; and several of the most 
       important kinds of interaction between two (and even three
       or more) stars. Some of the interactions discussed are 
       Roche-lobe overflow, tidal friction, gravitational 
       radiation, magnetic activity driven by rapid rotation, 
       stellar winds, magnetic braking and the influence of a 
       distant third body on a close binary orbit. A series of 
       mathematical appendices gives a concise but full account 
       of the mathematics of these processes. 
588 0  Print version record. 
590    eBooks on EBSCOhost|bEBSCO eBook Subscription Academic 
       Collection - North America 
650  0 Double stars|xEvolution.|0https://id.loc.gov/authorities/
       subjects/sh92002195 
650  0 Multiple stars.|0https://id.loc.gov/authorities/subjects/
       sh85088378 
650  7 Double stars|xEvolution.|2fast|0https://id.worldcat.org/
       fast/897107 
650  7 Multiple stars.|2fast|0https://id.worldcat.org/fast/
       1029040 
655  4 Electronic books. 
776 08 |iPrint version:|aEggleton, P.P. (Peter P.), 1940-
       |tEvolutionary processes in binary and multiple stars.
       |dCambridge, UK ; New York : Cambridge University Press, 
       2006|z0521855578|z9780521855570|w(DLC)  2006299123
       |w(OCoLC)61757144 
830  0 Cambridge astrophysics series ;|0https://id.loc.gov/
       authorities/names/n42034737|v40. 
856 40 |uhttps://rider.idm.oclc.org/login?url=http://
       search.ebscohost.com/login.aspx?direct=true&scope=site&
       db=nlebk&AN=165327|zOnline eBook via EBSCO. Access 
       restricted to current Rider University students, faculty, 
       and staff. 
856 42 |3Instructions for reading/downloading the EBSCO version 
       of this eBook|uhttp://guides.rider.edu/ebooks/ebsco 
901    MARCIVE 20231220 
948    |d20190507|cEBSCO|tEBSCOebooksacademic NEW 4-5-19 7552
       |lridw 
994    92|bRID