Online text: www.jirka.org/ra/html/sec_rintprop.html

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Cited passages: Section 5.2, Lemma 5.2.7 and Theorem 5.2.9.

Online text: www.jirka.org/ra/html/sec_rint.html

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Cited passages: Section 5.1, Example 5.1.4.

A conjugate base is what remains after a chemical acid donates one proton. In the conjugate acid-base pair $\mathrm{HA}/{\mathrm{A}}^{-}$, $\mathrm{HA}$ is the conjugate acid of ${\mathrm{A}}^{-}$; accepting a proton reverses the conversion. For example, acetic acid $\mathrm{C}{\mathrm{H}}_3\mathrm{COOH}$ loses a proton to give its conjugate base $\mathrm{C}{\mathrm{H}}_3\mathrm{CO}{\mathrm{O}}^{-}$. Partners differ by one proton and one unit of electric charge; they need not always be neutral and negative. Hydronium/water and water/hydroxide are also conjugate acid-base pairs.

At a prescribed pH, the ideal dilute acid dissociation constant determines the partition of a monoprotic acid inventory between its chemical species:These dimensionless fractions sum to one. They are the weak acid dissociation fraction and its complement when the only acid-bearing chemical species are $\mathrm{HA}$ and ${\mathrm{A}}^{-}$. Equal fractions occur at $\mathrm{pH}=\mathrm{p}{K}_a$ in this ideal approximation. For nonideal chemical solutions, equality of thermodynamic activities need not mean equality of concentrations.

For stipulated pKa $5$, the conjugate base fractions at pH $4$, $5$ and $6$ are $1/11$, $1/2$ and $10/11$. Here an external reservoir sets pH; its ions must supply the additional electric charge balance. The diagram omits those ions and water populations. It does not represent three pure $\mathrm{HA}$ samples at identical analytical concentration with freely chosen pH. In the latter experiment, the weak acid mass and charge balances determine pH as well as the partition.

The intergalactic medium is the gas between galaxies. Its diffuse, ionized component contains much of the ordinary matter outside stars. Lyman-alpha absorption measures its small neutral-hydrogen fraction, while hotter phases require other tracers.

Stellar parallax is the apparent change in a star's viewing direction caused by the observer's changing position. Nearby stars shift more against a distant reference background. In an ideal circular Earth orbit, the conventional annual stellar parallax $p$ uses a baseline of one astronomical unit, approximately the Earth-Sun distance. Two opposite observing positions, about six months apart, are separated by approximately two astronomical units. Their maximum angular separation is $2p$, so $p$ is half that excursion, not the full January-to-July shift. The observed excursion depends on the projected baseline and observing dates. ^[ref].

For the perpendicular baseline in the diagram, a right triangle giveswhere $p$ in the final expression is in radians. Combining the small-angle approximation with the parsec convention givesThus $p=0.05$ arcseconds implies $d\simeq 20$ parsecs, while the ideal six-month excursion is $0.10$ arcseconds. Geometry supplies this distance without assuming a luminosity or a particular stellar atmosphere.

In practical astrometry, many observations separate the annual stellar parallax signal from proper motion, the star's own changing sky position. The Gaia DR3 catalogue reports stellar parallax and its uncertainty in milliarcseconds: $50\mathrm{mas}=0.05$ arcseconds. A catalogue angle is a fitted measurement with measurement error. ^[ref].

For a positive stellar parallax with small standard deviation ${\sigma }_p$, first-order propagation gives ${\sigma }_d/d\simeq {\sigma }_p/p$. Thus $p=50\mathrm{mas}$ with ${\sigma }_p=1\mathrm{mas}$ gives $d\simeq 20$ parsecs with ${\sigma }_d\simeq 0.4$ parsecs, assuming systematic offsets are negligible. This linear estimate requires ${\sigma }_p\ll p$; a reciprocal is nonlinear and does not generally preserve symmetric uncertainty intervals.

A point-like astronomical source has an angular extent negligible for the calculation or measurement being considered. The ideal mathematical limit concentrates its luminosity at one source-plane position. In gravitational lensing, this approximation permits divergent formal magnifications on a caustic; a finite source averages the magnification over its emitting area. An unresolved source need not have negligible size compared with the lens's caustic scale.

An array whose entries appear in nondecreasing order under a specified total order. The displayed inequalities allow repeated values.

For example, $(2,5,5,9)$ is a sorted array of integers. Inserting $7$ at index $3$ gives $(2,5,5,7,9)$: with spare capacity, first shift $9$ one slot right. Appending $7$ would violate the sorted array property. Updating an entry also requires preserving the total order, or removing and reinserting it in a suitable position.

The useful combination is order plus direct indexed access: binary search eliminates a whole interval of candidates at each comparison, giving $O(\log n)$ search time complexity under constant-cost comparisons and the array cost model. A sorted array is therefore attractive for many lookups between changes, while keeping it sorted can still require $O(n)$ shifting work per insertion. A sorted linked list has the ordering information but does not supply the same constant-cost access to a middle index.

Storage of a multidimensional array with the first index varying fastest in consecutive positions. In a two-dimensional array, each column is contiguous. Traversing a row-major array by columns does not change its storage into column-major order.

Storage of a multidimensional array with the last index varying fastest in consecutive positions. In a two-dimensional array, each row is contiguous. Row-major order is a layout convention; a program can traverse that array by rows or by columns. See the explicit address calculation in spatial locality.