Star Clusters| Star Clusters |
In General
* Distance determination: For
nearby clusters (10–100 pc), extended parallax, convergent point method; For
distant ones (100s of pc), apparent magnitude and color index; For globular
clusters, variable stars in them.
* Open clusters: They contain
hundreds of much younger stars (up to a few tens of millions of years old); They
are distributed in the disk of the galaxy, mainly in the spiral arms, and are more
easily dispersed; Examples are the Hyades and the Pleiades (both in Taurus).
@ General references: Elmegreen & Efremov AS(98) [formation];
Merritt ANYAS(05)ap [Kandrup's work on relaxation];
Cardona 10 [field guide];
de Grijs a1107-conf [birth, evolution and death];
Stahler PT(12)oct [birth and death].
@ Open clusters: von Hippel ASP-ap/05 [galactic];
Elmegreen ap/06-conf [hierarchical patterns];
Moitinho IAU(10)-a0911 [and the galaxy];
Converse & Stahler MNRAS(10)-a1002 [Pleiades, dynamical evolution simulation results];
Gieles & Portegies Zwart MNRAS(11)-a1010 [vs associations];
Pelupessy & Portegies Zwart MNRAS(12)-a1111 [embedded];
Salaris proc(14)-a1409 [rev];
news nat(14)aug [is the Hipparcos distance to the Pleaides wrong?];
Norris & Norris a2101-in [why 'Seven Sisters'?].
> Online resources:
see Wikipedia page.
Globular Clusters
> s.a. galaxies [and dwarf galaxies]; pulsars;
unified theories [velocity dispersion profiles].
* Idea:
Stable, population II objects (with low abundance of heavy elements), with hundreds
of thousands of stars and characteristic relative HR diagrams; We know almost 200
in the Milky Way galaxy, distributed mainly in the galactic halo, and many in other
galaxies (including the Magellanic Clouds); Many contain variable stars, for example
M3 and M13.
@ General references:
Hénon AA(61)-a1103,
AA(65)-a1103;
Meylan ap/99-proc [dynamics];
Leon et al A&A-ap/00 [tidal stripping];
Maccarone & Knigge A&G(07)-a0709 [compact objects, rev];
Cezario A&A(13)-a1211 [in MW and M31, ages and metallicities];
Benacquista & Downing LRR(13) [relativistic binaries];
Bel a1404 [new kinetic model].
@ Formation, evolution: Krauss PRP(00)ap/99-in [ages];
Zepf ap/03-in [evolution];
Bekki et al MNRAS(08)-a0804 [simulation results];
Cohen IAU(10)-a0909 [and galaxy formation/evolution];
Forbes & Bridges MNRAS(10)-a1001 [accreted versus formed in situ];
Renzini a1302-proc [formation];
Chantereau et al IAU(15)-a1408 [massive star archeology];
Charbonnel et al A&A(14)-a1410 [and first-generation stars];
Renaud et al MNRAS(17)-a1610 [two types];
Carretta a1611-conf [multiple stellar populations].
@ And dark matter halos: Ibata et al MNRAS(12)-a1210;
Boylan-Kolchin MNRAS(17)-a1705.
@ In the Milky Way: Harris a1012 [catalog];
Zaritzsky et al ApJL(16)-a1604 [Milky Way GCs hosted by undetected subhalos (dwarf galaxies)];
Binney & Wong MNRAS(17)-a1701 [modelling].
@ Specific types:
Zepf & Ashman SA(03)oct [young globular clusters];
Kissler-Patig et al A&A(06)ap/05 [large ones, vs dwarf galaxies];
Lee et al proc(11)-a1011 [wandering globular clusters];
Gratton et al A&A(11)-a1105 [different populations in Omega Cen].
@ Specific clusters: Caldwell et al ApJL-a1402 [hypervelocity globular cluster near M87];
Laevens et al ApJL(14)-a1403 [the most distant MW globular cluster known];
di Tullio & Zinn AJ(15)-a1503,
Mackey et al MNRAS(16)-a1604 [search for Intergalactic Globular Clusters in the Local Group].
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send feedback and suggestions to bombelli at olemiss.edu – modified 26 jan 2021