Cisnull Pride Flag

Cisnullity (cisnul/cisnull): cisgender nullity; claiming ones cisness within gender nullity.

It can be called specifically NuTNu/Nu2Nu or 0t0/020 (zero to zero)/␀t␀/␀2␀/∅t∅/∅2∅.

Love a resident cat called Pickles at our Airbnb @thegherkinlevenshulme #manchester. Once I would’ve been horrified to have a cat in my close vicinity but I don’t seem to be allergic these days. It’s a wet and cold morning in #levenshulme but we are enjoying the quirky warmth of our home for these 4 nights. #winterinengland (will go in search for coffee soon) (at The Gherkin) https://www.instagram.com/p/CmtL_--NuLX/?igshid=NGJjMDIxMWI=

Stay home rock🤘🏾 I want to play on stage 🎸 . . . . . HP・Youtubeあります❗️プロフィール欄のリンクから飛んでください💁‍♂️ @yoshiaki_imahori https://instagr.am/p/CAhnii-nULx/

fact the grammarically null gender(s) always existed in all languages I see

Learn about upgrading your livestreams with the right gear. #livestream #contentcreator #facebooklive #podcast #gear #tech #graphics (at Atlanta, Georgia) https://www.instagram.com/p/BtCY-NulX-C/?utm_source=ig_tumblr_share&igshid=16wpgtzbuto7t

#this #enoughsaid https://www.instagram.com/p/BqdBC9-nULx/?utm_source=ig_tumblr_share&igshid=1tj2yuajadfbl

nulx is a cool dude. He's tall, dark and handsome. His fractals are, dare I say it, 'whack'. Well, they will be. When he posts them. Eventually. One day.

Sensnull Pride Flag

Sensnullity: refers to when one relates to the transnull experience, but only sometimes, temporarily, or not completely. Also known as sensnullgender (sens-null-gender or sens-nullgender), nullsensgender (null-sensgender), sensgendernull (sensgender-null).

[transcript: 5 stripes of black, dark grey, gray, light grey, and black. end id.]

Population synthesis of ultraluminous X-ray sources with magnetised neutron stars. (arXiv:2010.03488v3 [astro-ph.HE] UPDATED)

A model of population of ultraluminous X-ray sources with magnetised neutron stars (NULX) in a spiral galaxy with the star formation history similar to that in the thin disc of Milky Way is computed using a hybrid approach. First, applying analytical approximations (code BSE) we construct the ensemble of close binaries (CBS) which can be potential precursors of NULX. Next, evolution with accretion onto magnetised neutron stars (NS) is computed by the evolutionary code MESA. Accretion rate onto NS and X-ray luminosity are calculated for the models of sub- and supercritical discs and for the discs with advection. During accretion onto magnetised NS, super-Eddington luminosity $L_\mathrm{X}>10^{38}$ erg~s$^{-1}$ is attained already at the subcritical stage, when the energy release at the inner boundary of the disc defined by the NS magnetosphere is sub-Eddington. It is shown that standard evolution of CBS with an account of the peculiarities specific for accretion onto magnetised NS allows us to explain quantitatively observed characteristics of NULX (X-ray luminosities, NS spin periods, orbital periods and masses of visual components) without additional model assumptions on the collimation of X-ray emission from NS with high observed super-Eddington luminosity. In a model galaxy with star formation rate 3--5 $M_\odot {\rm yr^{-1}}$ there can exist several NULX. Discovery of a powerful wind from NULX with $L_{\mathrm X} \sim 10^{41}$ erg~s$^{-1}$ would be a signature of super-Eddington accretion onto magnetised NS.

from astro-ph.HE updates on arXiv.org https://ift.tt/3lsQWSx

Population synthesis of ultraluminous X-ray sources with magnetised neutron stars. (arXiv:2010.03488v2 [astro-ph.HE] UPDATED)

A model of population of ultraluminous X-ray sources with magnetised neutron stars (NULX) in a spiral galaxy with the star formation history similar to that in the thin disc of Milky Way is computed using a hybrid approach. First, applying analytical approximations (code BSE) we construct the ensemble of close binaries (CBS) which can be potential precursors of NULX. Next, evolution with accretion onto magnetised neutron stars (NS) is computed by the evolutionary code MESA. Accretion rate onto NS and X-ray luminosity are calculated for the models of sub- and supercritical discs and for the discs with advection. During accretion onto magnetised NS, super-Eddington luminosity $L_\mathrm{X}>10^{38}$ erg~s$^{-1}$ is attained already at the subcritical stage, when the energy release at the inner boundary of the disc defined by the NS magnetosphere is sub-Eddington. It is shown that standard evolution of CBS with an account of the peculiarities specific for accretion onto magnetised NS allows us to explain quantitatively observed characteristics of NULX (X-ray luminosities, NS spin periods, orbital periods and masses of visual components) without additional model assumptions on the collimation of X-ray emission from NS with high observed super-Eddington luminosity. In a model galaxy with star formation rate 3--5 $M_\odot {\rm yr^{-1}}$ there can exist several NULX. Discovery of a powerful wind from NULX with $L_{\mathrm X} \sim 10^{41}$ erg~s$^{-1}$ would be a signature of super-Eddington accretion onto magnetised NS.

from astro-ph.HE updates on arXiv.org https://ift.tt/3lsQWSx

Population synthesis of ultraluminous X-ray sources with magnetised neutron stars. (arXiv:2010.03488v1 [astro-ph.HE])

A model of population of ultraluminous X-ray sources with magnetised neutron stars (NULX) in a spiral galaxy with the star formation history similar to that in the thin disc of Milky Way is computed using a hybrid approach. First, applying analytical approximations (code BSE) we construct the ensemble of close binaries (CBS) which can be potential precursors of NULX. Next, evolution with accretion onto magnetised neutron stars (NS) is computed by the evolutionary code MESA. Accretion rate onto NS and X-ray luminosity are calculated for the models of sub- and supercritical discs and for the discs with advection. During accretion onto magnetised NS, super-Eddington luminosity $L_\mathrm{X}>10^{38}$ erg~s$^{-1}$ is attained already at the subcritical stage, when the energy release at the inner boundary of the disc defined by the NS magnetosphere is sub-Eddington. It is shown that standard evolution of CBS with an account of the peculiarities specific for accretion onto magnetised NS allows us to explain quantitatively observed characteristics of NULX (X-ray luminosities, NS spin periods, orbital periods and masses of visual components) without additional model assumptions on the collimation of X-ray emission from NS with high observed super-Eddington luminosity. In a model galaxy with star formation rate 3--5 $M_\odot {\rm yr^{-1}}$ there can exist several NULX. Discovery of a powerful wind from NULX with $L_{\mathrm X} \sim 10^{41}$ erg~s$^{-1}$ would be a signature of super-Eddington accretion onto magnetised NS.

from astro-ph.HE updates on arXiv.org https://ift.tt/3lsQWSx