PoS(CPOD07)062 / s a.it of on siss re- ys- ys- and sig- t gers stars Most sities ven gence pos. r micro- phases ratio mer act diagram p:// xtract impac discussed. the astroph astroph eme e (QCD) gers. t star proposed htt of of ferent Hea comp to high-den phase the mer dif at tron to Future amics rties used lution matter critically star mass-radius QCD neu The o the significan rotating v be odyn e leads or a state. prope are the the tron nsity e for structure al of in of v will the stars. e w . v neu stars ha Licence. chrom radii e re rich tion and ik data tron a high-de and transition star windo acility will determine f ntum als equa neu in ploration ae e ition phases stars, neutron v x v e qua tron and orkshop will re phase AIR and tic satellite F W of the matter neu xo stability ens rfs e al v and a to the ursts neutron superno rans on order e b matter transitions at dw hea collapsing of T quark ion-NonCommercial-ShareAl se -mode These ut r first the e llapse symmetry the x-ray . pha from in white Attrib telescop of of Internation nced detector vity cross-check and constraints strong ti interacting properties chiral 4th out core-co A enha Commons fness matter ankfurt.de Future e nt and Phas besides patterns CBM the v the nduc ysik d. se an stif e matter crucial as to v the stars, Creati in a a oph strongly ents den stars the profiles tic stars. w the fineme of of l ∗ in of ct outline xo such superco tron h vide e line Germany related QCD results terms strain are pro Decon for sics, the neutron tral color y compa con measurem of stro.uni-fr program Physik/Astr diagram vitationa y Main, of of under to ät –Bielic matter the proto-neu transitions he se r Spec Gra sit signals on am mass r se as literature transitions Onset normal astroph therefore pha able vy-ion etisc author(s) of amily quark to f pha furt rn be or the the QCD. sical stars. can and hea of y Unive n haffne nsity by nomen . pulsar phase in e se ank ls The int ared act r v er t the third from systems 2007 Sc mode e o to data F wned phe sics tly o schaffner@a P den a y für 8 en Goethe Speak high-de The ical due the recen Astroph cen of ph comp nals with of comp ical will 9-13 yright Darmstadt,German ∗ g . W Cop . uly c E-mail:

Jür Institut Signa J D-6043 GSI J Critical PoS(CPOD07)062 , in of the the the the vy- and and and eral state liquid v of ypical of a baryon hea hadron critical se strongly T of –Bielich potential after a not probe s of of imprint the the diagram high fner 5 density f ersion − temperatures Interestingly an by at mical transition proto-neutron v least ysics. will phase, e location ]. 10 with v Scha che equation temperatures ae, [1 line phase not v certain small the lea rk densities phase properties gen ut a the plasma astroph xplored b about at µ high modern e qua a Jür for in can to ulk and at at A is nuclear b be densities Darmstadt last superno and chiral transition w phase T the erse the QGP will lo v and MeV GSI the phase temperatures Color the at phase at to uni transition estimates 50 transition solid high-density densities. ratures Superconductivity similarities the of liquid the captures the for systems, early phase because phase anishing acility Plasma phase lore core-collapse the of related f tempe v as temperature equilibrium the xp c g of number e striking Quark−Gluon are transition. ferent non µ (QCD) in ysical FAIR of AIR interest QCD strong the dif ferent high range F phase, will are a associates are and dif 2 lines the temperatures phase ysics baryon of the and the and neutron stars astroph for one ens ph at entirely in There that and if simulations is phases . reach particular the 1 so Darmstadt densities QCD in Heav these N density (QGP), all of is well xistence CBM transition ure) of e , m / 3 the gers is all GSI Fig. nuclei chromodynamics of uperconducting and in the transitions at In in -s baryon press mer where baryon phase deconfinement plasma RHIC, LHC density diagram temperatures AIR ingredient, phase star F the high Hadrons Here, diagram with CERN encountered QCD. colour point ansition quantum program small etched QCD r at the of to early universe at T phase of at of sk of the m matter the se xtreme not is phase e the triple ations. neutron essential density LHC a vy-ion matter ysics quark-gluon at Pha with of that c progra line(s) ph an T en the hea QCD and diagram diagram T the v nuclear etch observ temperatures the as e QCD QCD of guments diagram sk the replace y-ion Note, matter is The es ar of v . the A with and densities phase phase of 1 oduction hadrons. ysical course, hea of 1: olution, serv transition normal (just phase v e of There Of The The e part high bang. program 1 Intr The ater . as. µ densities and Figur Signals densities. 1. interacting w g phase QCD properties phase star (EoS) big densities astroph ion this endpoint times symmetry PoS(CPOD07)062 xt. vy- star The EoS stars with solar signals hea xplode, Stairs). –Bielich conte e compact standing inclusion updating xtremely discussed to constitute e hole. eight fner codes, not f neutron nuclear this the and an Ingrid compact of a in stars possible olving as the of did in Scha signals black thereby v e of v of a relations in of mass ged hole) gen to xplosion, ution list simulation Jür transport, matter e models with massi courtesy emer of outline impact mentioned the black by a ], as scenarios simulations. has An contrib quark sequence and entually that w to Earlier v [11 neutrino e compact xposition this role ysics ]). successful e EoS future main ysical of a [8 from strange then generations in location. en These collapse w on e.g. astroph topic and ne beforehand, a. astroph (tak w possible nuclear Boltzmann xact v not see zero-age e to the in generate vie xplored of star the a the e w re ed be the ], 3 does supplementary be can vie [9 olv superno a re with case, found surements not v to ens apologise will e I y (and high-density be general mea an star ens modelling Heav in a has raised v wn a this, recent In can as ae the a proto-neutron instability remains do ]. mass of hea ae v and purposes w complete; v in QCD ] an [10 6 hot (for the core-collapse our of nor – a cools pulsar in ysics e that [3 v ysics the densities superno account for to simulations, ph SASI role superno ansition xplosions in star r fields e of radio T On out, oph a the of v se fices xhausti of xtreme e transition found astr suf e missing Pha collapses be turned be instability of magnetic aftermath research. superno it study core-collapse phase QCD , range core-collapse under can of and proto-neutron more, of the Compilation shock the The In neither three-dimensional or in 2: of QCD the ]. question field ysics e can [2 recently e If Matter ]. ph first the v successful High-density the rotation [7 born Figur is accretion Just for so of the modelling for temperature in 2. Signals masses Ref. ion objects. here acti PoS(CPOD07)062 , a a a

]. is ge to

of be on the se. for for the the the the the ery M is and one The vity to M been v lar stars ] been [17 ) at (there at of system 69 which star with per e . ] just masses normal (a nuclear used redshift , neutron only –Bielich v 1 [11 with has used

least a relati a xist [14 0002 ha out quite pulsar be matter M ger e . be companion xtracted total fner the at through and 2 f e 0 see Thanks assumptions a or neutron pulsars. capabilities). corrected A lar to limit , were could its e >  neutron the star can 2 relying ]. km normal either v that ruled alia arf pass the Scha a together general announced M ut B1516+02B data masses pulsars quarks ation b be dependent by [12 10 es be radius time. state mass vity of on from to 4414 measurement binary Fig. of w gen . which massi G of inter times reported 1 pulsars. of ne not ( were neutron in Jür star curv and solar are , star pulsar relati ation observ only might determined binary relation = of white-dw limit mass upper er model data substantially radii can four v probability input a the w as system. radio w M 1.40 property adius mass limits the them due w we en is ne as constant ne unconfined , sensational, y to layer to v adius mass observ and future assessment neutron data. articularly more stars which e star y e of depicted ge equations neutron 99% with Ho general oldest A P k are , ypical o a be of ] a on star w T is lar mass binary ]. be that uses ]. the mass-r wer are tw 1.14 man the . is outer the fe of star measurements ] [16 w Finally lo y ybrid mass-r One from [13 a [15 of the ould J h of the out critical . can a an ne sk come. ) [19 neutron for with w vitational modern

matter measured a stars or the σ there in to first J0621+1002 outlook a pulsars and ], M the that only (2 EoS. gra fects star periastron rule or with case, pulsars, range between for redshift 77 5I observing F ef used

hand, the . companion in [18 masses ut y stars result of been just 1 b double the more M not for in to companion ]. by an radio pulsar accretion is 5 a ed 4 results w y stars and . neutron the a Indeed, y 0748–676 2 Ref. en wn erzan do for In

other to solar no of [20 be neutron results than latter v the If T due quark ens of . ances moments), − M man incompatible In a gi ]. scans . densities kno 6 of km the with . mass observ one has the the 73 due adv ]. ephemeris confidence . e also 1.80 1 EXO be high-density of that be demonstrates are lines 8 Heav 2006 [21 2 g star . precisely compact accurac are mass binary a On = ws to 1 er the ed the one greater [19 pulsars radio mass motion of the the and will  ould 68% core the M there to in Ref. sho pulsar e the in urst , and 8 from aver w a the of directly quite stars, v . 1.53 clearly b folding 3 systems of The quadrupole to e mass the spectral of observ principle neutron pulsars It and 13 pulsar v confirmed of a abo added). arf EoS gi in ]. in with aylor median of detailed from ≥ eplerian If viour ybrid the being radius x-ray en mass a ansition K h claimed dw R has ]. in v Figure r [19 precisely radio years determining reader on-line space-time M ar T were pulsars. range gi data as f binary history as the measured the beha that w another of could the [17 comparable of 26 se of a with and . compilation nuclear on the the fe masses density Hulse-T so stars it , of 1 el be or quite core. J0751+1807 analysis on vities 1600 data

the well v –white Pha stars M le last star from soft w arf as that The acti the being on with can the refer companion solar arpage only 28 ne than mass . recent . I olutional the amous in ge w of ery limits pulsar QCD o 0 f combining to v pulsar constraints constraint to neutron ] confidence material v analysis e stars in procedure assumption lar the tw  a from in neutron the conference by the the once solely [19 which , the neutron More so to the 10 rather of density of er the white-dw 68% flurry J1748–2021B of mass . problem adius adius three be ered matter in of v for is 2 v confidence a a corrections quark a recent A Present uncertainty densest opposed , , mass one we ≥ the fects as xtracted xtracted details. determine mass star matter Signals the the of star recent center ef pure depends its M The quark might disco during w rotating promising Montreal detected pulsar made with mass-r mass e Ho (as mass e mass-r of 99% Under pulsar PoS(CPOD07)062 a ct by for the not and soft- not adius e is quark -mode within matter masses r e interest particle –Bielich compa pressure stability ursts freedom v of b about enhanced quiescent ge w of of the , fner stars the possible mass-r f phase, ne pressur lar w quark total EoS inside massi long w and of are gree substantial Scha ery , the 15 ne there the wledge v a de , xotic’ e windo systems rather strange quite amma-ray gen er star matter ’e to w kno g between v in for on be ne case, Jür masses an we a 14 emission, wering presence ysical and quark ge ybrid lo can as Ho matter orks h stability result (poor) the . ]), lar completely softer w either relation a

that x-ray a include Hybrid (2SC+DBHF)

can

[26 stars 13 M for In to EXO 0748-676 EXO astroph the and is 1 Hybrid (2SC+HHJ) quark e . ] late -mode 2 wing r present s therefore classic of star a,

of [25

quark σ v becomes ]). sho en QCD.

hand

an quarks signals 1 12 our v the and condensation, of [18 literature to Blaschk densities, pure ith EoS stars mass hea els transitions, other neutron the Some v W vid since superno due from rid kaon a 11 le between a in The the appearance the That Da acuum yb en 5 or of approaches v h baryon ).

phase least

in of σ on

3 the 2 (tak ens Radius R [km] at of Fermi and pulsars maximum 10 vial both systems. high freedom. without Fig. correct. wn ution Neutron star (DBHF) radii in Heav at yperons )) proposed phase of 2 collapse stars h in s relates matter Interactions nontri α kno the not and 9 typical rk ysical signals as w-lying rotating , a in e (GRBs the contrib lo matter wn. quark grees v qua similar signals a been de w quark i.e. the for with masses 8 astroph matter The collisions, Quark star (QCD O( ] actually has rapidly unkno matter calculation Hybrid, mixed (CFL+APR) ge . ansition in filling r . 24 it is (see T lar it star – misconception strikingly se interacting relation numerous 7 hadronic to QCD stars stars, strange nuclear quark w). constant, [22 vitational density depth stars be e

result, rather Pha 0.8 which 1.6 0.4 2.4 2.0 1.2

in v basically the Mass M [M ] [M M Mass gra to wn been w belo bag neutron for is ybrid auli to e ne or h do common P v EoS strongly model QCD out strange F ws the baryon (see compact ha neutron transition of w of to Mass-radius the the bag allo en ne by of perturbati of binary appearing l v wn density of rather 3: turns a of stars etc.). e addition gi en e stil phase the A There v gy a MIT Hunting olv a gi v particularly for ening opens mere Figur Signals properties ener stars species (see the a is or matter relation quark 3. cooling transition times spin-do in PoS(CPOD07)062 2 s in is or or α for and v that than both same 4 more out using about (free) based model QCD, apless of y g a neutron –Bielich insights o-fla actually is ed to matter order the lines) neutrino- a are es Fig. Note, is in tw d rather constant fner man ork in to of f dense in mainly ed w 1 basic km, curv lines (CFL), up quark of stars bag matter density and fix Scha core wn 12 phase, past Fig. for been be Some of sho gen the MIT in QCD phase (long-dashe quark symmetry the erage has is in Jür e not v approaches. ]). EoS quark v ed a the transition in part. hadronic properties 33 pure 15 first. mass-radius radius e.g. ent the of can details). model – equilibrium chiral the lock a stars) of fer depicted the β for phase from or [29 , bag normal that stars ] i.e. alue v dif in v , nature from perturbati with hadronic 34 3 ange modelled and see applications , lines -fla in R diagram

MIT underlying relation vity (str quark [25 M ∝ implies 1 the quarks: been using . color the chosen 10 M transition 2 ysical see density phases phase pure stars a the Interestingly on has w realized of originates completely the literature . transition the within lo is the of is Λ and lines, phase, on radius µ the of in astroph 6 mass-radius statement the quark =3 alues uperconducti =145 MeV based QCD stars v Λ calculation 1/4 phase the there -s to Radius (km) for point ens phase 2SC (solid B original a The this matter transition 2 s 5 patterns pure , . α despite more and quark the that dense xistence color with crucially for Heav location , reach e QCD for which apless µ in stars are quark g phase the (for of the pure order =2 =200 MeV the and can matching , from other Λ pairing in 1/4 phases to subtraction B er ]) for clear its pure v that depends ations QCD 24 increases phase stars relation the as tion fects (2SC), neutron each , not we assumption Unfortunately 0 ferent ain ef diagram transition is the . to ansition estig Ho 0 1 2 [23 r mass ag relation dif CFL it well v

mass T the

of 0.5 1.5

quark sun star calcula phase in radius true M/M to as se sed Besides or phase (see of close that ordinary star considering the ]. Pha due so QCD mass- renormalisation stres for by The , notion ery metallic e guments! [28 v v mass maximum ay Modern that as model be mass-radius ar model incorporating the QCD the w . and ] lie found, compact of The The the bag typical bag proto-neutron [27 alues act, matter xtracted undetermined f v of a e 4: should matter perturbati in The superconducting been e phase, In It The or be MIT MIT maximum choice e ]. symmetry v the the typical constant. approaches within on independent star quark [25 Figur Signals the incorporating equally color CFL deconfinement. trapped detail can ha the PoS(CPOD07)062 e at of of as so for the the and , lik first first neu- vita- bare, radii, stars. x-ray ], stable phase ysical where strong of of for precise relation present –Bielich gra unusual 46 matter’) solution a possible terms amily ed common possible. xtremely is transition triggered ent f transition , late at and minimum a matter e solution of transition), ] w twins, from , constant fner pulsars a kind ypothesises anishing f fer mix as are that h ne [45 more with strange astroph v y The [49 , colliding density a dif with third unfortunately). star clear . bag an phase phase to be (’quark , Scha with o the amily a stable non phase are gy f also masses a radii o econd arfs) just not tw transition is for vity T w which possibilities the from hadronic or traditional emission mass-radius matter ursts J1739 gen e pulsars that . stars is dw b ener true radii ne for chiral es to gra luminosity and pulsar has phase third there Jür it the The v the a the of compact a star , ge with means twin no phase similar by XTE the holds, the w to er quark the Note, xtreme lar is v e that possible pressur sub-millis e that amily v with Or to of critical star stars. matter neutron f at not is That o (strange masses we ybrid scale of ha y include so restored the chiral h stick spin-up of amma-ray ut binary tw core. , , the there star (note generate Ho g Eddington I ]). b strange - specifically arfs star). ybrid , the starts to quark quark ypothesis vitational h small are stars vity or ables (or [43 second h radius a can If dw possible and x-ray stars ersion gra xistence gra super frequenc chirally matter are density ], stable v the e star see so-called neutron are and interactions as there ], match by order neutron a gy a observ [47 the , relation con white wing. matter called the , 36 matter 1 proposed simplicity Strange only by spontaneous to properties. of amily , quark w-mass ], f stars ones, well arbitrarily ener mass the compact or first rotation lo proportional strange follo not from ]. F the light adius [35 Fig. has 7 bound ace as [42 to of a km. matter is quark pure the and strange possible ordinary the the third the [44 signals of a ens are surf of and one finite composition, due collapse core to e.g.: in 200 the stabilised sometimes the of a (an mass-r weakly compact hadronic relation (in)stabilities if from ∼ Heav as crust) is Other relation the of model stars at is phase of diagram, core star ents transition stable. matter’). types ysical the small R star ]. v xplosions, stars equations the similar e xist e xistence matter frequencies f e e bag at scenario the e stars a stars in [48 from CFL signal that their consists -mode of v v scaling both radius types r

phase radii, also the a neutron anishes solution so possible astroph o strange M by of corresponds the only that olk v to , MIT ypothetical 1 a transition w compact -superconducting . a h tw times eal -V to absolutely and 0 (’hadronic xplosi amily rotation mass- v hadronic f ansition QCD selfbound account can e realistic eral of the to due r superno 1122Hz is crust, neutrino compact re v ∼ stable T follo Note, really a color the then in one se density 2SC (also the chiral are ordinary of for ]. se and w M y , consists into es due e stars type of third and pressure of y ] more ursts v e gy masses en ne 42 by the b (ignoring a of could the limiting matter quiescent Pha – ordinary the the star e , nuclear curv w been the [37 one tak distinguished within v amily ation ener star a brok a e the quark f -rays, as This to anishes [38 v from be γ long and w frequenc contrast, mass feature QCD v relation just is that transition origin of which quark stars ha first-order Either while probably shock In is es, has pure the can and third . v observ stars , a suggested this are the star ]. compact radii. a olman-Oppenheimer of a twin’ er there chirally adius ables anishing transition matter core w compact T phase at as or v generic, one v [22 there F The There stars mass-radius the if strange strange pressure transition 2 vitational we the the the strongly / reanalysis non 1 rising Signals quite starts that matching. order quark Ho features here, in to The is then solutions that and smaller secondary the phase observ B order hot whether neutron the tron a to compact mass-r a small gra and/or tional emission ’ PoS(CPOD07)062 - of e.g all the by the the Jo- ury The ards with This ation of color hand, range insta- rotate Array w of ]. detec- radius double system are es, atories system release (UNO) (see optical, –Bielich satellite to to a subclass Sudb ordinary es. elescope y detectors or the [48 the v ark the T can F a is P outside sk xtended the fner other observ the xperiencing in temperature f for stars This the e w -mode atory e ]. ge then for on observ r unstable in matter points ursts ]. the e the the future special temperatures b [54 Lar and Scha successor v and be Kilometre well star matter and aii a a o which in [53 ations ferent shocks w confirmation w for On certain is Observ tw ery gen the Arecibo, (LISA) quark and which dif compact a those V inner ould gime Ha , ents for vitational the Jür so-called ant is w v of quark re in the v Square at e constraints observ boosted the e it gra There compact e huge with the at and detected, . case a v ast be rele transition) the measured f of is between neutrino with similar typical field gi vitational Antenna (JWST), by as getic be -Kamiokande day x-ray e the futur w hence, v collapsing will gra yperons) and viscosity temperature. been , ation will stars h ener per phase for be quite elescopes ha elescope, rotate then or Space T strong Super T the measured aited. ulk prospects near satellites has telescopes this seconds) are b emission xcluded areas w of elescope with decay e as be once transitions ould a matter the stars only eck T observ which 40 could highly w (chiral the holes and K the en in Space are compact radio v can J0737-303) these as elescope, can in well ferent to xciting (e pulsars around QCD about than T the e dense radio ursts vity Space the all dif as y eagerly b These black Nucleon only neutron matter neutrinos. ge of star gions due 8 quiescence are telescopes (PSR is in ysics for and as which a both both Hubble Interferometer to re QCD ebb v , occur measured, (more Lar matter ph ens Relati that telescopes of of W wton, of the ysics ursts. ] after be quark ities , such b and ground of v These frequenc atory pulsar Laser star Ne rapidly Other to Heav . system spectra. times [52 compact amma-ray ae neutrino and can Accreting ferent superno g v K proposed signal ens, the satellites: James wn release the significantly . by v General 8 dif the Under atories collapsing urst sensiti the first signals microph the in do Extremely b Observ gy XMM- 10 of pulsar number the to the hea rotation and neutron the before of ables radio inertia the alactic amma-ray therein). and ws = The the to matter superno ge stars g quiescent XEUS, ener limit, and the not of T Observ tests on slo the and ysical of high lar of ursts ansition in ations and xtrag of and double r a b a submillisecond observ atories e The long source and T es, Southern a stars, quark o star epler amma-ray best . oph v transitions: thanks at Ordinary (SNO). Bank ones g a demonstrated se en K VIRGO, tw where . v wing. w QCD references moment with for Chandra the e observ depends as astr the sources ysical observ Pha time, the w and of matter engine of w from phase atory stable to elescope, the possible follo Green and stars urst or accreting -mode and presently it neutron e the of T , r f higher b compact ] European v vides A temperature QCD first are an standard the optical or and astroph are for a inner [50 the windo the pro vitational LIGO, satellites the of in the Observ Constellation-X K w the similar at the hunt matter for xtracted Space to 8 neutron of stars detection gra fe of e Indeed, systems telescopes, properties i.e. (see or engine. o ast Bank, , 10 Colliding There A F of f consecuti gies x-ray T) amma-ray listed the ]). The the tw that g present o = dormant ybrid xistence h respect T that e [51 nuclear ener instability characteristics bility of candidates tw a range inner Signals Besides superconducting of pulsar 4. (VL of are of Hubble missions (SKA), at drell the tion GEO600, for future Neutrino PoS(CPOD07)062 a to of of be vi- wn for the the ace uni- EoS lead core than 10% for third to adius using ariety of mass- gra bright detec- a kno for radius. clearly v normal to surf core strange neutron EoS –Bielich rotating the e detector ger is by of 5 is v of vitational vitational vitational to the space-time a in the could to confidence lar the the matter fner matter rich emission of mass-r f w transition gra gra gra of to just a pattern y en in xpected CBM binary future v e the to signal e from the Scha precisely strong the quark a is listen’ 99.9% quark EoS the such xistence , opportunities polytropic mass ’ the phase ursts, be a sizable e on successfully and , b gen the transition lead a ery a of accurac simulations matter of to nonspherical the v comparison the vitational instabilities with core, Jür ratio in by (the w an with of in state of within could lots modelling originate simple limits Gra nuclear from measurement phase Clearly of a applied matter Quark w star In a years with are wn’ quark ness -mode the ae. ratio windo Remarkably already f ne r visible ]. v xample: a ics. amma-ray ]. to fects numerical signal e relation which g limited w been on is to adopt ys QCD stif the background ef be modified set ybrid [61 [64 , is ne h There due for 1.95. mass-radius with eral equation The has a coming the and due are v ursts touch-do just adius star The to ould b ’ superno ae. to se dense limit y to be, the v w the astroph determined gers stars ]. authors interest signal radius include 75 e binaries, in . stars lines to v in and are entirely e star 1 be wn The nuclear of x-ray [68 and v mass-r mer method relation The a ens. before The = an model-independent detectors. v ybrid compact w by the can erse ]. superno h Γ x-ray ]. which ybrid a v star sensiti The 9 There h up es hea 67 xotic ]. to the of spin-do spectral of pulsar e , neutron data. ]. [60 as uni ]. of x ens transitions based of suspected high-density

the [68 59 possible inertia [66 GEO600). the the , the [47 e.g. M black-holes, stars wn highly between in collapse ae Constellation-X inde background neutron used 4 of es x-ray are vitational to Heav opened . and v ations mass-radius are in literature deformations of v [58 by e themselv and 1 emitted space phase be a urst v and be ordinary ith y es gra the a ge b w core of v wn the has the to eal W a the w e an in ysics close spin-do v lar binary of mass neutron v relation observ w the ealed in on . present a then re kno stars LIGO of superno of moment future ph v detectors out arious adiabatic compactness In of w v mass of re accurac II The the (as The an can the stars can frequencies the ]. ations x-ray be with vitational getting ansition sustain w If The turns 5% r ]. ysical ]. type vy-ion 63 vitational astronomy T ), on profile to neutron reported no ]. material , gra with stars collapse 57 act using 57 vitational e constraint f one-to-one se collapse shape gra v hea – assumed – densities. higher [54 vitational observ a spectrum [62 stars. stars The by gra in a signal The within compact pulsars w right

Pha an . astroph the [55 e gra es [55 phase tight signals , of ]. M and v entional to v detectable high of depends of densest ) a a neutron a v star for unique colliding emission 7 could ourier at w [65 w ( a vity be QCD with spectral wn between able e F the stars con v is compact km collision, compact generate ysical a vide do matter Finally the characteristic 7 which and . stars, vitational w of stars 3381 stars the observing relati for Sources . of of ]. 6 relation could J0437–4715 pro arped neutron star matter 1 emission check observ emissions will in wed w 67 Accreting Gra There > are e es e = quark one probing , Summary vitational vitational earth neutron v v v astroph the an R will A arpage a a a erse. amily general The to w it neutron of radius Signals of narro pulsar w to M quark tational neutron v gra tors seen gra quark the [66 produces neutron stars w the 5. relation w cross- on f of for PoS(CPOD07)062 ” . , ion and and se pro- their y and of 7A, stars . v 2.1 star Ingrid matter olter 49, se ) –Bielich ct for A for W to “ hea 328 act –288, of H. fner SN198 agliara, 2–12 state ol. f QCD and (2005 and P v /0303171 Collap 193 compa comp of Drago Core-Collap of ) 124 and Grigorian, ears 31 after , of Cordes, ) Scha sics Y of eds., G y h/0407149 H. indebted Core . measurements ation 2810 M. eber gen (2005 ysics logy ory years J. (2005 modern am W ersations equ Thirty ph Giuseppe Jür . 54 Phys. I v Stairs, astro-ph F : astroph . mass Stellar ar . , and J “The and 634 y y , the , . H. Alessandro ” omeno Gaitanos, con of , astro-p . 01, J . twenty sk sk I. Phys. w 3+16 ls from T dings. /0602038 on nucle 5. . s, phen pulsar the Hempel, 2411 S265 rvie and Müller thank 200 Kramer e ) B191 soft densities state Nucl. ophys. arXiv:0708. v Mode in I the losions B. a procee o ” Fuch +. oskresen M. of 12072 ed xp V , Astr numerous art. S259– Rasio v e ral C. “Is high (2003 P nucl-th and ” 25– , from , Pulsar . D. tion these at A. data?, en g Matthias , 90 discussions for matter . v o 02, gene pp. to F ssler , Jessner , state unpublished (2006) Pr “Impro equa A particular . s Sturm, inedo, Decay state ae ” Lett. Binary A. of 0358 F pulsar ar . 32 thank in rümper C. , quark of v ution ) . r I and T fruitful Series G trino-dri A. 10 , stars: Re stars, , y J. Pulsar for astro-ph/06 and with nication. Frankfurt ation nucle vistic Orbital in ens ation e, (2006 act 4, ence “Neu Kifonidis, contrib in r Löhme Phys. man equ the Martínez-P recent Phys. . Dalen 74 r Finally Radio J K. [nucl-th] Relati Heav ” O. “Equ vistic Röpk G. 38–7 patible C commu for ” comp an matter e signals . v conference, -Bielich, Confe . v [nucl-th] the G. ration, and group most ate din, , , Kitaura, nuclea E. “Th and Re v Relati in ific fner Binary Stairs, incom l, this quark (2007) San Marek, pri af the pulsars, star ac by .-S. in friends Missing?, . (2007). H. 8.4216 P constraining F F ylor, Janka nsity ype collabo Miller ” A. possible Phys. is a data 412215 . I. T Sch on 442 matter manuscript. T T , ” e, the and sis, . . radio M. of J. and ansition and S. 06.0130 er Stairs, during ion , r o-ph] H. H. v of v the T of CBM “Strange e, ank , What Rept. high-de J. list quark ty compact progress Measured vy- se to Analy and update [astr Spla the eitse sses 08050 07155 Ingrid the nt Klahn, Lang Marek, and ietoska, hea . the collisions, . arXiv:070 Pha long M. Socie for Phys. g and Rampp T W on ” Blaschk K. A. s ” “Ma colleagues a and losions: olom -Bielich, Pulsar , , astro-ph/0 .3056 years E. arXiv:07 e, e, K “Rece “Strange M. D. from M. a ” y-ion , gments QCD from w v r detailed Exp s, my eisber fner tions, v E. Friese ation f rt, Nice a fe with Mass a Janka Janka corrections W Nice, –657, Stairs, the rno no er . . ebe hea onomical Ho, Blaschk J. Buras, Fuch vid wled Klähn, of W me Scha M. Sage H. last for ences olk . . thank xtracted Sagert astro-ph/05 Solar Supe astro-ph/04 Astr observ Still arXiv:0706 Observ e [astro-ph] A. and reactions, “Constraints S651 R. F H.-T D. V I. J. C. T Da D. H.-T I. J. I the [9] [7] [8] [6] [1] [5] [2] [4] [3] [14] [13] [10] [11] [12] collaboration. Refer Irina clarifying Stairs viding in Signals Ackno PoS(CPOD07)062 . ) . lan, in ” s. high urst . , 205, 121 see v color b e neutral neutral ) (2006 sity Kap (2005) in v –Bielich 7, 09073 Re 2 sity Phy ti 441 of of g L. and matter den ” e 307 fner 200 den X-ray (2003 f (1986) D. ark 7, 4 ce Phys. arfs, 04, high the Natur ” breakin , Physics perturba 160 and high Scha dw diagram diagram in ” “Qu , B56 e in droplets 12–1 0340 at Scien . se se n st ” gen hep-ph/05 , from matter Lett. white lines ophys. pha pha 261 Natur Kaspi, . Jür stars Matter 25, ) rk ensates s. ” se . (2005) Augu ct symmetry -Bielich, stars M. Nucleo Astr . l, qua Star Phy “The “The 72 den . V 0340 cond elescope 396 (1986 ” fner on. , T e, e, ed D of sity: . af chiral . k compa quark . tron v 272. absorption 310 Astr Bose den /0211126 of se . . Sch 03 Re -lock Montrea ” (2006) and Ban J ductor information, class Neu n rk Rischk Rischk Camilo, J. 711395 or . s. den ication. v w 73 F ing for H. H. class (1984) stars, ne . Phys. D -fla and baryo w 01143 . Green Inside ” D. D. ophy /0606524 rk 30 v redshifted lock “Diqua Pulsars’, supercon , hep-ph/9711 State D Re the color “Ne “Small, y astro-ph Freire, or qua lly . Astr liara, 0077 commun and and of v finite v sics: of s. , , sk ” ss 53, hep-ph/9 y C. ag y y te Possible rs v ge 54, at masses, -fla , Re ) a v v P color o v o o ea Phy A 11 r C. Using hep-ph/98044 “ k k . o Y tions ” G. . 51– elk Stars, 247 , v v pri P 5 v astro-ph , r ) . ens V dings. -Bielich, -Bielich, vitationa ) hep-ph/01 “Gaple e “Stran , (1998 astroph Phys. quark “Color “QCD , ’40 443, Sho Sho ” ebe o-fla Equa M. of 81 fner fner fer pal, f f “Gra erzan Heav W t tw Klähn (2002 A. A. (1998 Stairs, Stairs, nce . T ef clear procee . trapping, z, E7–E8 F and I. I. Soft “Strang nucl-th/011 T 702(R), 0311286 the ilczek, ilczek, H. in Lett. . Scha Scha (1999) phases, 420 422 . “Nu I. W W pless Scha v in lla, lla, Rajago e out and J. J. trino . . 121 these B of Ingrid 223, , h/0605106 ryak, confere F F ) Re treatmen 537 Mende R. 21. (2006) K. to “Ga Olinto, Drago, neu and and B , Pulsars Buba Buba and the Shu Natur Lett. M. and and 217– Rules and . of ettner A. A. and 445 ” hep-ph/ 9–35 at , (2001 , Hessels, nd V Phys. ansition M. M. K Lattimer, ution e r e, . n ” and T Nice Phys. k T . . e E. 63 and fect Huang star 351 C. eco separation Phys. . astro-p v aris, M. , 001, 8-676 gopal, gopal, , ph/0501230 ef se D Pisarski, Pisarski, (2002) ” erth, erth, gi W , 5) vid J. . M. Natur fer Zdunik 142 184 v 17, ouv W W contrib tron 222 arhi, J. Nucl. 074 D. D. ” . . Da aerels, Pha Raja Raja Blasch K Self-consistent The Millis F ) vity L. ” Re talk e, nning P V V and (199 and R. R. neu A702 Schä . , , J. C. K. K. D. E. instantons, , , 5–11 y F . “Cosmic a astro- a a 74 g. v T stars?, ducti k, QCD “EXO o (2004 alter QCD, of Phys. 111 .or k and p, Blasck ct Kasian, matter: matter: Freire, Glende Ransom, Phys. v W ” Rüster Rüster Frag Frag nty-One 92 itten, the 444. 896, Lett. . Alford, Alford, Alford, Alford, K. Rap Alcoc vid S. S. W B. B. M. v of M. Özel, we Haensel, Cottam, Sho aolo . . . hep-ph/0302 density Lett. Nucl. Re supercon matter hep-ph/0503 QCD, quark quark 443– “T spectra ns2007 892– compa (2006) E. N. I. M. M. Laura Da E. R. C. P M. E. S. S. S. F M. P J. F [34] [35] [32] [33] [31] Signals [15] [26] [25] [30] [24] [23] [29] [22] [27] [28] [16] [21] [18] [17] [20] [19] PoS(CPOD07)062 , a ” s. in , . s. 758, and for , ) of and rsus stars ophy e . v of Phy rk –Bielich ers, 463 Lorimer matter 747– ” ) 353 lk stars Astr ) tron (1981 ratory . qua instability D. fner ” s. uu Inner (2006) f Urca millisecond 14 0401086 eron neu amily structure of K -mode f tron Stars, X-Ray r (2000 A in Labo (2006 yp m ophy E. stars, h Scha G32 0611716 s. ghlin, by neu -mode 05145 r . Star to d third 450 matter: Astr in timing Rare A677 tron gen Phy a Dormant rotating s. diagra the . Götz, Strange rk Phys. a s. A J of on. Jür the in . McLau neu - ” J D. e of induce 03016 astro-ph/ and qua . in ophy Phy ” instabilities phases Neutron Bare M. Astr phase and transition g ” etti, . gr-qc/04 Hz 57, rk astro-ph/ Stars, Astr ursts the , Hints the ment gh b System xistenc cores, Nucl. oun . 60, e e -mode strange on. ” in Y wins, 3–11 r transitions v “Qua 1122 nsed matter . T a Camilo, , “Phase from L100 0005490 of nfine the 12602 Mere of . se at , by w 3–10 Astr 115 F s l Bursts: stars , ) S. e ” Star ity y and deco le-Pulsar dense Conde L97– 105 astro-ph/07 v “Pha 01772 ) Thoma 9912418 es tron Curv transitions, Greiner (2004 hester rotating viscosity Lund, . H. cold siti timing, Pion 004, ducti Doub . strange-matter quark vitationa W Oscillations (2007 in (2006) ulhon, Neutron N. A 303 M. astro-ph/ star den of “ 3. Light 125 gra and t, Manc phase go ) with Gamma-Ra “Bulk and ce protoneu rt 12 astro-ph/05 657 445 pulsar act 01, rk , nal tical R. and . 160 04275 for Burst e, and in of er ) 4, clear supercon ens arfs Gour astro-ph/ Brand Freire, and Qua ensation “Sho (2007 Scien “Sig Lett. 1711 . 1325 comp astro-ph/07 E. dw , . ” S. P imes le es r core ophys. 13, –123 J , 75 Stöck (1997 A Heav T color Rischk X-Ray “ olution ak cond s. -Bielich, D Possenti, and supranu ebe sics, 013, and hiani, nt 10– H. signature Astr 79 “Non-Iden Stab . . H. y the Ev Hz 1227 v ) white (2002) , and W . at Zand a (1968) A. r e, quark ) fner . of sel, ophy Ph in 125 D. , renti, on. I. Re F e of as 89 “Pion af ) a corequ Lett. Berez usk rmal 172 P , nolds, astro-ph/02 . stars 1122 state (2007). ettne (2000 M. Astr . v y and Astr “Th and Z. I. v Sch Haen (2007 K , “Quiesce ” , 807155 of J. of ” Lett. stars . ´ Phys. y nski, Re e 85 Re alysis J. (2007 P . Kramer Re Hana “The Plasma v 101, . . ” C. J. v , ansition , , o J. and and Pei, 665 r o-ph] v An nce 75 . -285, Possibility stability T “ M. Re M. pact strange stars, vk ation J 131 S. and Lett. , , gliara, and Phys. D orn, , ph/0604366 320. . y Prószy se a Phys. Uso . v the a ” [astr 2) rid al. liara, liara, Blaschk , P v . Bejger Sho com ” Joshi, 09806 01467 g Greiner ding, vity V J1739 Re M. “Equ “Evide yb Phys. et ag ag Pha Re D. . wn G. of , 306– processes, h A. B. P P M. nning nning ophys. ” C. Priesk (200 “On Bur V ) , ben , Gra -Bielich, . stars, , I. ws ic .1510 “Probing astro-ph/9 of and G. G. Z. and astro- XTE and 89 M. , , Phys. Astr d, se fer QCD and Phys. stars, msick, fner ” ” in wn L9, , f amily’ e, ertler back ” spin-do (1982 o L475 , f Gerlach Glende Glende Sa’ vistic ge T Mathe lepton the 760, Zdunik Lett. yn a . D’Amico, J. H. P K. Sch Drago K. Drago L Drago Kämp A. v of Sand Haensel Kaaret, 258 A. Scha L. Madsen, ransient . . . . third superden Re 747– (2000) L471– J ’ astro-ph/05 astro-ph/00 arXiv:0704 spin-do cores: pulsar N. Relati neutron matter non- T pulsars, J. Engine G. U. D. B. P N. K. A. N. J. J. B. A. A. A. F P J. Signals [36] [38] [37] [39] [40] [41] [42] [47] [45] [43] [46] [51] [52] [53] [48] [44] [49] [50] PoS(CPOD07)062 , the of ” 75 s. JCAP of D from and X-ray . ” high Phy –Bielich AIP stars, v on reting ” rstanding Inertia 617 at ” Lorimer ests . Re rk . the fner J . . stars, of f acc from 80. “T s. D. , state, qua y Inertia emission “Unde a Bursts, se-transition matter Phy tron of -3039A,B Scha e rties 9–14 g from of transition ” v ophys. 512419 08105 t 09447 a pha neu ardt, Camilo, 146 Bur Moment w gen strange . ) X-ray quark J0737 in Astr Prope stars, ations F constraining Jür phase ” M. e . from of v “The equ s Momen n, and Star 102, Markw e ce (2004 binary v Using oscillations State, tic QCD de, a pulsars B. vitational . 97– of massi already with w xo 349 of of e C. transitions astro-ph/0 . urst 6) gra of al influen Ferdma Freire, State b astro-ph/05 astro-ph/05 . 7, e Neutron P tion binary on Soc R. of State haripan and orbits fects LIGO nce h/0411470 with (200 , 02039 , and 6). on phase “Th of 635, 382, the on. –276 and “Ef “Is vitation Equa bou yne P 314 ation . . of limits nolds, L stars “Last nn, (200 a, lines aints Lamb y , Astr from R. ce er 2765 and lear A. . “Gra Equ act str d Re ) . (2005) K. (2006) R. , V . astro-p . amad elsson, 2791 J. Equation F inertia Nuc ulhon gr-qc/07 Y Scien “Upp Star 364 639 and “Con comp Not. , ” Suen spectral ghlin, go of Thielema bs, , (2006 er, . S. 0401465 the , 13 [gr-qc] 984, the kgroun 01, J Samu collapse 03399 al. of 11127 K. . 38 nts ace ens Soc. . Hob piro, and et bac L. .-M. Gour h o-ph/061 Mon. F . 979– pulsar 0420 c e W McLau ” r Neutron G. . v on. surf tions E. Sha ophys. sional a and Heav astr Grindlay and ble Strohmay of w M. ” nstraining the L. and “Mome 8.2984 Astr gers, , E. and Abbott Astr E. the . (2005) Resea , (2007) dou of S. 0411353 astro-ph/ . ” J. Constraining “Co B. , gr-qc/04 s T in mer Jones, ce deforma 0602345 Chu, 702476 Roy Hashimoto, osyan, o-dimen the 629 hester I. tz, and astro-ph/05 D76 Pulsars, . arte, 12, Sarkissian, analysis stars, tw C. J Spa . star –252 i, Haensel, vitational v D. Probe J. Not. . nd mg Pogh in P M.-a. Miller, M. Schu elastic Re Manc oration, 101, . -3039A: gra 245 0640 ansition , , . tron timing arXiv:070 from r G. eco e ) F s. ek-Rosinska C. Bau ces T R. ” ophys. , and . astro-ph/ 211 rsson, Mon. ¯ through neutron u, Rybick neu B. se ” M. W “Future Phy otak imum J0737 astro-ph/ 5) from Collab of . B. , Cheng ry Astr , 38, logical 09417 Millis (2004 (2005) ” K Gond Ury astro-ph/0 D’Amico, T ” Advan and Ande Pha Stairs, QCD? S. G. yer Bulik, of EOS, K. 71 ” D. radiation matter vity K. (200 002 , N. . bina “Max I. s 714 N. nts, v of aryya, ) 5–L1 T K. Pulsar , 012, , e, D , 95 k . on r no rs ll, pulsars, sity QCD v collapse oc. “Cosmo stars, e relati 084 L13 ation Scientific hslin, d Lin, matter Re Pr Lattimer (2006 Strohma Owen Morrison, the . Lett. ral asuta Binary . Kramer Bejge vitational radio Possenti, Y Sigl, Hask J. Oec Bogda Bhattach v E. of Limousin, M. A. . . induce gra neutron gene Phys. 0604 astro-ph/06 (2007) high-den A. Conf Observ the dense Measureme densities paramete Re 78 (2004) N. G. M. F L.-M. S. M. I. LIGO B. S. B. T J. R. [67] [68] [57] [65] [66] [60] Signals [54] [55] [61] [63] [59] [62] [58] [56] [64]