pdgLive

ASTR

Fuzzy DM

$<1.9 \times 10^{4}$

⁴

BAUMHOLZER

COSM

warm dark matter

⁵

CROON

ASTR

SN 1987A, axion-muon coupling

⁶

FUJIKURA

ASTR

Microlensing

⁷

MARTINCAMALIC..

ASTR

SN 1987A, ${{\mathit \Lambda}}$ decay

$\text{none } 1.3 - 2.7 \times 10^{-13}$

⁸

ASTR

BH superradiance

$>2 \times 10^{-20}$

⁹

ROGERS

COSM

Lyman-$\alpha $

$\text{none } 0.8 - 6.5 \times 10^{-13}$

¹⁰

TSUKADA

ASTR

BH superradiance

$>2 \times 10^{-17}$

¹¹

IRSIC

COSM

Isocurvature fluctuations

¹²

PODDAR

ASTR

Compact binary systems

$>2.1 \times 10^{-21}$

¹³

SCHUTZ

COSM

Fuzzy DM

$\text{none } 6.4 - 8.0 \times 10^{-13}$

¹⁴

SUN

ASTR

BH superradiance

$\text{none } 2.9 - 4.6 \times 10^{-21}$

¹⁵

DAVOUDIASL

ASTR

BH superradiance

$\text{none } 10^{-21} - 6 \times 10^{-20}$

¹⁶

MARSH

ASTR

Fuzzy DM

$\text{none } 1.1 - 4 \times 10^{-13}$

¹⁷

PALOMBA

ASTR

BH superradiance

$<0.06$

¹⁸

2018

ASTR

K, SN 1987A

$<0.67$

¹⁹

ARCHIDIACONO

2013

COSM

K, hot dark matter

$\text{none } 0.7 - 3 \times 10^{5}$

²⁰

CADAMURO

2011

COSM

${}^{}\mathrm {D}$ abundance

$<105$

²¹

2011

CNTR

D, solar axion

²²

CAST

K, solar axions

$<0.72$

²³

COSM

K, hot dark matter

²⁴

CAST

K, solar axions

$<191$

²⁵

CNTR

K, solar axions

$<334$

²⁶

KEKEZ

HPGE

K, solar axions

$<1.02$

²⁷

2008

COSM

K, hot dark matter

$<1.2$

²⁸

2007

COSM

K, hot dark matter

$<0.42$

²⁹

MELCHIORRI

2007

COSM

K, hot dark matter

$<1.05$

³⁰

2005

COSM

K, hot dark matter

$3\text{ to }20 $

³¹

MOROI

1998

COSM

K, hot dark matter

$<0.007$

³²

BORISOV

ASTR

D, neutron star

$<4$

³³

KACHELRIESS

ASTR

D, neutron star cooling

$<(0.5 - 6){\times }\text{ 10}$$^{-3}$

³⁴

KEIL

ASTR

SN 1987A

$<0.018$

³⁵

1995

ASTR

D, red giant

$<0.010$

³⁶

ALTHERR

1994

ASTR

D, red giants, white dwarfs

³⁷

1993

ASTR

K, SN 1987A

$<0.01$

1992

ASTR

D, white dwarf

$<0.03$

1992

ASTR

D, C-O burning

$\text{none 3 - 8}$

³⁸

BERSHADY

ASTR

D, K, intergalactic light

$<10$

³⁹

KIM

COSM

D, K, mass density of the universe, supersymmetry

⁴⁰

ASTR

D,K, SN 1987A

$<1 \times 10^{-3}$

⁴¹

RESSELL

ASTR

K, intergalactic light

$\text{none } 10^{-3} - 3$

ASTR

D,K, SN 1987A

⁴²

ENGEL

ASTR

D,K, SN 1987A

$<0.02$

⁴³

ASTR

D, red giant

$<1 \times 10^{-3}$

⁴⁴

ASTR

D,K, SN 1987A

$<(1.4 - 10){\times }\text{ 10}$$^{-3}$

⁴⁵

ERICSON

ASTR

D,K, SN 1987A

$<3.6 \times 10^{-4}$

⁴⁶

MAYLE

ASTR

D,K, SN 1987A

$<12$

CHANDA

ASTR

D, Sun

$<1 \times 10^{-3}$

ASTR

D,K, SN 1987A

⁴⁷

ASTR

red giant

$<0.07$

FRIEMAN

ASTR

D, red giant

$<0.7$

⁴⁸

ASTR

K, red giant

$\text{< 2-5}$

TURNER

COSM

K, thermal production

$<0.01$

⁴⁹

DEARBORN

ASTR

D, red giant

$<0.06$

ASTR

D, red giant

$<0.7$

⁵⁰

ASTR

K, red giant

$<0.03$

ASTR

D, white dwarf

$<1$

⁵¹

KAPLAN

1985

ASTR

K, red giant

$\text{<0.003 - 0.02}$

IWAMOTO

1984

ASTR

D, K, neutron star

$>1 \times 10^{-5}$

ABBOTT

COSM

D,K, mass density of the universe

$>1 \times 10^{-5}$

DINE

COSM

D,K, mass density of the universe

$<0.04$

ELLIS

ASTR

D, red giant

$>1 \times 10^{-5}$

PRESKILL

COSM

D,K, mass density of the universe

$<0.1$

BARROSO

ASTR

D, red giant

$<1$

⁵²

ASTR

D, stellar cooling

$<0.07$

ASTR

D, red giant

LAGUE 2022 used the BOSS galaxy-clustering data to set limits on the abundance of ultralight axion dark matter. When combined with the CMB data, they obtained $\Omega _{{{\mathit A}^{0}}}\mathit h{}^{2}$ $<$ 0.004 for ${\mathit m}_{{{\mathit A}^{0}}}$ = $10^{-31} - 10^{-26}$ eV. See their Figs. 1 and 15 for mass-dependent limits.

²	YUAN 2022A use the data of Advanced LIGO and Advanced Virgo's first three observing runs to search for stochastic GW background produced by scalar bosonic clouds formed by the BH superradiant instability. They set the limit, taking into account all the unstable modes.

³	BANIK 2021 use the subhalo mass function inferred from the analyses of the GD-1 and Pal 5 stellar streams. The limit is strengthened to $2.2 \times 10^{-21}$ eV when adding dwarf satellite counts.

⁴	BAUMHOLZER 2021 study the freeze-in production of axion dark matter through couplings to photons, and set the limit using Lyman-$\alpha $ forest data and the observed number of Milky Way subhalos.

⁵

CROON 2021 study the supernova cooling effect of the axion-muon coupling, taking account of semi-Compton scattering and muon-proton bremsstrahlung, as well as the loop-induced axion-photon coupling, and exclude the range of $\mathit g_{ {{\mathit A}} {{\mathit \mu}} {{\mathit \mu}} }$ $\simeq{}$ $7 \times 10^{-3} - 2 \times 10^{-10}$ for ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ $0.5$ GeV. See their Fig. 8 for mass-dependent limits.

⁶

FUJIKURA 2021 use the EROS-2 survey and the Subaru HSC observation to set limits on spherically symmetric axion clumps, taking account of the finite lens and source size effects. $\mathit f_{{{\mathit A}^{0}}}{ {}\gtrsim{} }$ $10^{12}$ GeV can be constrained depending on the fraction of the axion dark matter collapsed into clumps, and the clump densities. See their Figs. $7 - 10$ for the limits.

⁷

MARTINCAMALICH 2021 considered axion emission from a supernova core through the ${{\mathit \Lambda}}$ hyperon decay, and set the limit on B( ${{\mathit \Lambda}}$ $\rightarrow$ ${{\mathit n}}{{\mathit A}^{0}}$ ) ${ {}\lesssim{} }$ $8 \times 10^{-9}$, or equivalently, $\mathit f_{{{\mathit A}^{0}}}/C_{sd}{ {}\gtrsim{} }$ $2.6 \times 10^{9}$ GeV in terms of the flavor-violating axion coupling to the down and strange quarks.

⁸	NG 2021 use the binary black holes reported by LIGO and Virgo to determine the black hole spin distribution at formation and the scalar boson mass simultaneously, neglecting the boson self-interaction.

⁹	ROGERS 2021 set the limit by using a framework involving Bayesian emulator optimization to accurately forward-model the Lyman-$\alpha $ flux power spectrum, and comparing this with small-scale data to constrain the predicted suppression of cosmic structure growth.

¹⁰	TSUKADA 2021 look for a stochastic GW background produced by extragalactic BH-hidden photon cloud systems through the superradiant instability. They assume a uniform spin distribution at birth of isolated BHs from 0 to 1.

¹¹

IRSIC 2020 used the Lyman-$\alpha $ forest constraint on small-scale isocurvature perturbation to derive limits on the axion mass and decay constant, assuming that the axion makes up all dark matter in the post-inflationary scenario. See their Fig. 1 for other astrophysical limits as well as the limits on the case of the temperature-dependent axion mass.

¹²

PODDAR 2020 used the observed decay in orbital period of four compact binary systems to derive a limit on the emission of axions with ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ $1 \times 10^{-19}$ eV, assuming they couple to nucleons and the strong $\mathit CP$ phase vanishes at the potential minimum. They exclude $\mathit f_{{{\mathit A}^{0}}}{ {}\lesssim{} }$ $10^{11}$ GeV for such axions.

¹³	SCHUTZ 2020 set a limit on fuzzy dark matter based on the existing limits for warm dark matter derived from the inferred subhalo mass function.

¹⁴

SUN 2020 look for quasimonochromatic gravitational waves emitted from boson clouds around the Cygnus X-1 black hole. The quoted limit assume the black hole age of $5 \times 10^{6}$ years. A mass range of $9.6 - 15.5 \times 10^{-13}$ eV is disfavored when repeated induction of bosenova for string axions with decay constant $\mathit f_{{{\mathit A}^{0}}}$ $\simeq{}$ $10^{15}$ GeV prevents the superradiance from being saturated.

¹⁵	DAVOUDIASL 2019 used the observed data of M87* by the Event Horizon Telescope to set the limit. A mass range of $0.85 - 4.6 \times 10^{-21}$ eV is disfavored for a spin-1 boson.

¹⁶

MARSH 2019 considered heating of star clusters due to the stochastic oscillations of the core and granular quasiparticles in the outer halo. The limit was derived by requiring the survival of the old star cluster in Eridanus II, where the lower end is set by the validity of diffusion approximation. The effect of tidal stripping is also discussed for lower masses.

¹⁷

PALOMBA 2019 used the LIGO O2 dataset to derive limits on nearly monochromatic gravitational waves emitted by boson clouds formed around a stellar-mass black hole. They exclude boson masses in a range of $1.1 \times 10^{-13}$ and $4 \times 10^{-13}$ eV for high initial black hole spin, and $1.2 \times 10^{-13}$ and $1.8 \times 10^{-13}$ eV for moderate spin. See their Figs. 2 and 3 for limits based on various values of black hole initial spin, boson cloud age, and distance.

¹⁸

CHANG 2018 update axion bremsstrahlung emission rates in nucleon-nucleon collisions, shifting the excluded mass range to higher values. They rule out the hadronic axion with mass up to a few hundred eV, closing the hadronic axion window. See their Fig. 11 for results based on several different choices of the temperature and density profile of the proto-neutron star.

¹⁹	ARCHIDIACONO 2013A is analogous to HANNESTAD 2005A. The limit is based on the CMB temperature power spectrum of the Planck data, the CMB polarization from the WMAP 9-yr data, the matter power spectrum from SDSS-DR7, and the local Hubble parameter measurement by the Carnegie Hubble program.

²⁰	CADAMURO 2011 use the deuterium abundance to show that the ${\mathit m}_{{{\mathit A}^{0}}}$ range 0.7$~$eV -- 300$~$keV is excluded for axions, complementing HANNESTAD 2010 .

²¹	DERBIN 2011A look for solar axions produced by Compton and bremsstrahlung processes, in the resonant excitation of ${}^{169}\mathrm {Tm}$, constraining the axion-electron ${\times }$ axion nucleon couplings.

²²

ANDRIAMONJE 2010 search for solar axions produced from ${}^{7}\mathrm {Li}$ (478 keV) and ${}^{}\mathrm {D}({{\mathit p}},{{\mathit \gamma}}){}^{3}\mathrm {He}$ (5.5 MeV) nuclear transitions. They show limits on the axion-photon coupling for two reference values of the axion-nucleon coupling for ${\mathit m}_{{{\mathit A}}}<$ 100 eV.

²³	This is an update of HANNESTAD 2008 including 7 years of WMAP data.

²⁴	ANDRIAMONJE 2009 look for solar axions produced from the thermally excited 14.4 keV level of ${}^{57}\mathrm {Fe}$. They show limits on the axion-nucleon ${\times }$ axion-photon coupling assuming ${\mathit m}_{{{\mathit A}}}<$ 0.03 eV.

²⁵	DERBIN 2009A look for Primakoff-produced solar axions in the resonant excitation of ${}^{169}\mathrm {Tm}$, constraining the axion-photon ${\times }$ axion-nucleon couplings.

²⁶	KEKEZ 2009 look at axio-electric effect of solar axions in HPGe detectors. The one-loop axion-electron coupling for hadronic axions is used.

²⁷	This is an update of HANNESTAD 2007 including 5 years of WMAP data.

²⁸

This is an update of HANNESTAD 2005A with new cosmological data, notably WMAP (3 years) and baryon acoustic oscillations (BAO). Lyman-$\alpha $ data are left out, in contrast to HANNESTAD 2005A and MELCHIORRI 2007A, because it is argued that systematic errors are large. It uses Bayesian statistics and marginalizes over a possible neutrino hot dark matter component.

²⁹	MELCHIORRI 2007A is analogous to HANNESTAD 2005A, with updated cosmological data, notably WMAP (3 years). Uses Bayesian statistics and marginalizes over a possible neutrino hot dark matter component. Leaving out Lyman-$\alpha $ data, a conservative limit is 1.4 eV.

³⁰

HANNESTAD 2005A puts an upper limit on the mass of hadronic axion because in this mass range it would have been thermalized and contribute to the hot dark matter component of the universe. The limit is based on the CMB anisotropy from WMAP, SDSS large scale structure, Lyman $\alpha $, and the prior Hubble parameter from HST Key Project. A ${{\mathit \chi}^{2}}$ statistic is used. Neutrinos are assumed not to contribute to hot dark matter.

³¹	MOROI 1998 points out that a KSVZ axion of this mass range (see CHANG 1993 ) can be a viable hot dark matter of Universe, as long as the model-dependent $\mathit g_{ {{\mathit A}} {{\mathit \gamma}} }$ is accidentally small enough as originally emphasized by KAPLAN 1985 ; see Fig.$~$1.

³²	BORISOV 1997 bound is on the axion-electron coupling $\mathit g_{\mathit ae}<1 \times 10^{-13}$ from the photo-production of axions off of magnetic fields in the outer layers of neutron stars.

³³

KACHELRIESS 1997 bound is on the axion-electron coupling $\mathit g_{\mathit ae}<1 \times 10^{-10}$ from the production of axions in strongly magnetized neutron stars. The authors also quote a stronger limit, $\mathit g_{\mathit ae}<9 \times 10^{-13}$ which is strongly dependent on the strength of the magnetic field in white dwarfs.

³⁴	KEIL 1997 uses new measurements of the axial-vector coupling strength of nucleons, as well as a reanalysis of many-body effects and pion-emission processes in the core of the neutron star, to update limits on the invisible-axion mass.

³⁵

RAFFELT 1995 reexamined the constraints on axion emission from red giants due to the axion-electron coupling. They improve on DEARBORN 1986 by taking into proper account degeneracy effects in the bremsstrahlung rate. The limit comes from requiring the red giant core mass at helium ignition not to exceed its standard value by more than 5$\%$ ($0.025$ solar masses).

³⁶	ALTHERR 1994 bound is on the axion-electron coupling $\mathit g_{\mathit ae}<1.5 \times 10^{-13}$, from energy loss via axion emission.

³⁷

CHANG 1993 updates ENGEL 1990 bound with the Kaplan-Manohar ambiguity in $\mathit z={\mathit m}_{{{\mathit u}}}/{\mathit m}_{{{\mathit d}}}$ (see the Note on the Quark Masses in the Quark Particle Listings). It leaves the window $\mathit f_{\mathit A}=3 \times 10^{5}-3 \times 10^{6}$ GeV open. The constraint from Big-Bang Nucleosynthesis is satisfied in this window as well.

³⁸	BERSHADY 1991 searched for a line at wave length from $3100 - 8300$ $Å$ expected from 2${{\mathit \gamma}}$ decays of relic thermal axions in intergalactic light of three rich clusters of galaxies.

³⁹	KIM 1991C argues that the bound from the mass density of the universe will change drastically for the supersymmetric models due to the entropy production of saxion (scalar component in the axionic chiral multiplet) decay. Note that it is an $\mathit upperbound$ rather than a lowerbound.

⁴⁰	RAFFELT 1991B argue that previous SN$~$1987A bounds must be relaxed due to corrections to nucleon bremsstrahlung processes.

⁴¹	RESSELL 1991 uses absence of any intracluster line emission to set limit.

⁴²

ENGEL 1990 rule out $10^{-10}~{ {}\lesssim{} }$ $\mathit g_{\mathit AN}{ {}\lesssim{} }~10^{-3}$, which for a hadronic axion with EMC motivated axion-nucleon couplings corresponds to $2.5 \times 10^{-3}~$eV ${ {}\lesssim{} }{\mathit m}_{{{\mathit A}^{0}}}{ {}\lesssim{} }$ $2.5 \times 10^{4}~$eV. The constraint is loose in the middle of the range, i.e. for ${\mathit g}_{\mathit AN}$ $\sim{}~10^{-6}$.

⁴³	RAFFELT 1990D is a re-analysis of DEARBORN 1986 .

⁴⁴	The region ${\mathit m}_{{{\mathit A}^{0}}}{ {}\gtrsim{} }$ 2 eV is also allowed.

⁴⁵	ERICSON 1989 considered various nuclear corrections to axion emission in a supernova core, and found a reduction of the previous limit (MAYLE 1988 ) by a large factor.

⁴⁶	MAYLE 1989 limit based on naive quark model couplings of axion to nucleons. Limit based on couplings motivated by EMC measurements is 2$-$4 times weaker. The limit from axion-electron coupling is weak: see HATSUDA 1988B.

⁴⁷	RAFFELT 1988B derives a limit for the energy generation rate by exotic processes in helium-burning stars $\epsilon $ $<$ 100 erg g${}^{−1}$ s${}^{-1}$, which gives a firmer basis for the axion limits based on red giant cooling.

⁴⁸	RAFFELT 1987 also gives a limit ${\mathit g}_{\mathit A{{\mathit \gamma}}}$ $<$ $1 \times 10^{-10}$ GeV${}^{-1}$.

⁴⁹	DEARBORN 1986 also gives a limit ${\mathit g}_{\mathit A{{\mathit \gamma}}}$ $<$ $1.4 \times 10^{-11}$ GeV${}^{-1}$.

⁵⁰	RAFFELT 1986 gives a limit ${\mathit g}_{\mathit A{{\mathit \gamma}}}$ $<$ $1.1 \times 10^{-10}$ GeV${}^{-1}$ from red giants and $<2.4 \times 10^{-9}$ GeV${}^{-1}$ from the sun.

⁵¹	KAPLAN 1985 says ${\mathit m}_{{{\mathit A}^{0}}}$ $<$ 23 eV is allowed for a special choice of model parameters.

⁵²	FUKUGITA 1982 gives a limit ${\mathit g}_{\mathit A{{\mathit \gamma}}}$ $<$ $2.3 \times 10^{-10}$ GeV${}^{-1}$.

References:

LAGUE

2022

JCAP 2201 049

Constraining ultralight axions with galaxy surveys

YUAN

2022A

PR D106 023020

Constraints on an ultralight scalar boson from Advanced LIGO and Advanced Virgo?s first three observing runs using the stochastic gravitational-wave background

BANIK

JCAP 2110 043

Novel constraints on the particle nature of dark matter from stellar streams

BAUMHOLZER

JCAP 2105 004

Structure Formation Limits on Axion-Like Dark Matter

CROON

JHEP 2101 107

Supernova Muons: New Constraints on $Z$? Bosons, Axions and ALPs

FUJIKURA

PR D104 123012

Microlensing constraints on axion stars including finite lens and source size effects

MARTINCAMALICH

PR D103 L121301

Supernova Constraints on Dark Flavored Sectors

PRL 126 151102

Constraints on Ultralight Scalar Bosons within Black Hole Spin Measurements from the LIGO-Virgo GWTC-2

ROGERS

PRL 126 071302

Strong Bound on Canonical Ultralight Axion Dark Matter from the Lyman-Alpha Forest

TSUKADA

PR D103 083005

Modeling and searching for a stochastic gravitational-wave background from ultralight vector bosons

IRSIC

PR D101 123518

Early structure formation constraints on the ultralight axion in the postinflation scenario

PODDAR

PR D101 083007

Constraints on ultralight axions from compact binary systems

SCHUTZ

PR D101 123026

Subhalo mass function and ultralight bosonic dark matter

SUN

PR D101 063020

Search for ultralight bosons in Cygnus X-1 with Advanced LIGO

DAVOUDIASL

PRL 123 021102

Ultralight Boson Dark Matter and Event Horizon Telescope Observations of M87*

MARSH

PRL 123 051103

Strong Constraints on Fuzzy Dark Matter from Ultrafaint Dwarf Galaxy Eridanus II

PALOMBA

PRL 123 171101

Direct constraints on ultra-light boson mass from searches for continuous gravitational waves

2018

JHEP 1809 051

Supernova 1987A Constraints on Sub-GeV Dark Sectors, Millicharged Particles, the QCD Axion, and an Axion-like Particle

ARCHIDIACONO

2013A

JCAP 1310 020

Axion Hot Dark Matter Bounds after Planck

CADAMURO

2011

JCAP 1102 003

Cosmological Bounds on sub-MeV Mass Axions

2011A

PR D83 023505

Constraints on the Axion-Electron Coupling for Solar Axions Produced by a Compton Process and Bremsstrahlung

JCAP 1003 032

Search for Solar Axion Emission from ${}^{7}\mathrm {Li}$ and ${{\mathit D}}({{\mathit p}},{{\mathit \gamma}}){}^{3}\mathrm {He}$ Nuclear Decays with the CAST ${{\mathit \gamma}}$-ray Calorimeter

JCAP 1008 001

Neutrino and Axion Hot Dark Matter Bounds after WMAP-7

JCAP 0912 002

Search for 14.4 keV Solar Axions Emitted in the M1-Transition of ${}^{57}\mathrm {Fe}$ Nuclei with CAST

2009A

PL B678 181

Search for Solar Axions Produced by Primakoff Conversion using Resonant Absorption by Nuclei

KEKEZ

PL B671 345

Search for Solar Hadronic Axions Produced by a Bremsstrahlung-like Process

2008

JCAP 0804 019

Cosmological Constraints on Neutrino plus Axion Hot Dark Matter: Update after WMAP-5

2007

JCAP 0708 015

Cosmological Constraints on Neutrino plus Axion Hot Dark Matter

MELCHIORRI

2007A

PR D76 041303

Improved Cosmological Bound on the Thermal Axion Mass

2005A

JCAP 0507 002

A New Cosmological Mass Limit on Thermal Relic Axions

MOROI

1998

PL B440 69

Axionic Hot Dark Matter in the Hadronic Axion Window

BORISOV

JETP 83 868

Compton Production of Axions on Electrons in a Constant External Field

KACHELRIESS

PR D56 1313

Axion Cyclotron Emissivity of Magnetized White Dwarfs and Neutron Stars

KEIL

PR D56 2419

Fresh Look at Axions and SN1987a

1995

PR D51 1495

Red Giant Bound on the Axion $−$ Electron Coupling Revisited

ALTHERR

1994

ASP 2 175

Axion Emission from Red Giants and White Dwarfs

1993

PL B316 51

Hadronic Axion Window and the Big Bang Nucleosynthesis

1992C

PL B291 97

Constraints on Mass of the DFSZ Axions from the Carbon$−$Oxygen Burning Stage of Stars

1992

MPL A7 1497

Constraints of Axions from White Dwarf Cooling

BERSHADY

PRL 66 1398

Telescope Search for Multi-eV Axions

KIM

1991C

PRL 67 3465

Effects of Decay of Scalar Partner of Axion on Cosmological Bounds of Axion Supermultiplet Properties

1991B

PRL 67 2605

Multiple Scattering Suppression of the Bremsstrahlung Emission of Neutrinos and Axions in Supernovae

RESSELL

PR D44 3001

Limits to the Radiative Decay of the Axion

PR D42 3297

Axions and SN1987a: Axion Trapping

ENGEL

PRL 65 960

Emission and Detectability of Hadronic Axions from SN1987a

1990D

PR D41 1324

Axion Bremsstrahlung in Red Giants

PR D39 1020

Axions and SN1987a

Also

PRL 60 1797

Axions from SN1987a

ERICSON

PL B219 507

Axion Emission from SN1987a: Nuclear Physics Constraints

MAYLE

PL B219 515

Updated Constraints on Axions from SN1987a

Also

PL B203 188

Constraints on Axions from SN1987a

CHANDA

PR D37 2714

Astrophysical Constraints on Axion and Majoron Couplings

PRL 60 1793

Boundson ExoticParticle Interactions from SN1987a

1988B

PR D37 549

Bounds on Weakly Interacting Particles from Observational Lifetimes of Helium Burning Stars

FRIEMAN

PR D36 2201

Axions and Stars

PR D36 2211

Bounds on Hadronic Axions from Stellar Evolution

TURNER

PRL 59 2489

Thermal Production of not so Invisible Axions in the Early Universe

DEARBORN

PRL 56 26

Astrophysical Constraints on the Couplings of Axions Majorons and Familons

1986B

PL 166B 402

Axion Constraints from White Dwarf Cooling Times

PR D33 897

Astrophysical Axion Bounds Diminished by Screening Effects

KAPLAN

1985

NP B260 215

Opening the Axion Window

IWAMOTO

1984

PRL 53 1198

Axion Emission from Neutron Stars

ABBOTT

PL 120B 133

A Cosmological Bound on the Invisible Axion

DINE

PL 120B 137

The not so Harmless Axion

ELLIS

1983B

NP B223 252

Constraints on Light Particles from Stellar Evolution

PRESKILL

PL 120B 127

Cosmology of the Invisible Axion

BARROSO

PL 116B 247

Constraints on Light Axions

1982B

PR D26 1840

Astrophysical Constraints on a New Light Axion and other Weakly Interacting Particles